Researcher Database

Mitsuteru Sato
Faculty of Science Earth and Planetary Sciences Cosmosciences
Professor

Researcher Profile and Settings

Affiliation

  • Faculty of Science Earth and Planetary Sciences Cosmosciences

Job Title

  • Professor

Degree

  • Ph.D.(2004/03 Tohoku Univ.)

URL

Research funding number

  • 50312541

J-Global ID

Research Interests

  • Electromagnetic wave observations   Typhoon   Severe weather   Observations in Antarctica   Satellite measurements   Planetary Atmosphere   Transient Luminous Events   Lightning   

Research Areas

  • Natural sciences / Atmospheric and hydrospheric science
  • Natural sciences / Space and planetary science

Academic & Professional Experience

  • 2007/10 - Today Hokkaido University Faculty of Science Lecturer
  • 2007/09 - 2007/09 Tohoku University Department of Geophysics, Graduate School of Science
  • 2006/04 - 2007/08 RIKEN (Institute of Physical and Chemical Research) Computational Astrophysics Laboratory Special Postdoctoral Researcher
  • 2004/04 - 2006/03 RIKEN (Institute of Physical and Chemical Research) Computational Astrophysics Laboratory
  • 1998/04 - 2004/03 Tohoku University Department of Geophysics, Graduate School of Science Doctor course
  • 1999/11 - 2001/03 41st Japanese Antarctic Research Expedition Member of the wintering party
  • 1996/04 - 1998/03 Tohoku University Department of Geophysics, Graduate School of Science Master course
  • 1992/04 - 1996/03 Tohoku University Department of Science

Education

  • 1998/04 - 2004/03  Tohoku University  Graduate School of Science  Department of Geophysics
  • 1996/04 - 1998/03  Tohoku University  Graduate School of Science  Department of Geophysics
  • 1992/04 - 1996/03  Tohoku University  Department of Science

Association Memberships

  • The Meteorological Society of Japan   Society of Atmospheric Electricity of Japan   SGEPSS   American Geophysical Union   

Research Activities

Published Papers

  • Y. Wada, T. Enoto, Y. Nakamura, T. Morimoto, M. Sato, T. Ushio, K. Nakazawa, T. Yuasa, D. Yonetoku, T. Sawano, M. Kamogawa, H. Sakai, Y. Furuta, K. Makishima, H. Tsuchiya
    Journal of Geophysical Research: Atmospheres 125 (4) 2169-897X 2020/02/27 [Refereed][Not invited]
     
    ©2020. American Geophysical Union. All Rights Reserved. During 2017–2018 winter operation of the Gamma-Ray Observation of Winter Thunderclouds experiment in Japan, two downward terrestrial gamma-ray flashes (TGFs) that triggered atmospheric photonuclear reactions were detected. They took place during winter thunderstorms on 5 December 2017 and 9 January 2018 at Kanazawa, Ishikawa Prefecture, Japan. Each event coincided with an intracloud/intercloud discharge, which had a negative-polarity peak current higher than 150 kA. Their radio waveforms in the low-frequency band are categorized as a distinct lightning type called “energetic in-cloud pulse” (EIP). Negative-polarity EIPs have been previously suggested to be highly associated with downward TGFs, and the present observations provide evidence of the correlation between them for the first time. Furthermore, both of the downward TGFs followed “gamma-ray glows,” minute-lasting high-energy emissions from thunderclouds. It is suggested that the negative EIPs took place with downward propagating negative leaders or upward positive ones developed in highly electrified regions responsible for the gamma-ray glows.
  • G. Abdellaoui, S. Abe, J. H. Adams, A. Ahriche, D. Allard, L. Allen, G. Alonso, L. Anchordoqui, A. Anzalone, Y. Arai, K. Asano, R. Attallah, H. Attoui, M. Ave Pernas, S. Bacholle, M. Bakiri, P. Baragatti, P. Barrillon, S. Bartocci, J. Bayer, B. Beldjilali, T. Belenguer, N. Belkhalfa, R. Bellotti, A. Belov, K. Belov, K. Benmessai, M. Bertaina, P. L. Biermann, S. Biktemerova, F. Bisconti, N. Blanc, J. Błȩcki, S. Blin-Bondil, P. Bobik, M. Bogomilov, E. Bozzo, S. Briz, A. Bruno, K. S. Caballero, F. Cafagna, D. Campana, J. N. Capdevielle, F. Capel, A. Caramete, L. Caramete, P. Carlson, R. Caruso, M. Casolino, C. Cassardo, A. Castellina, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, G. Chiritoi, M. J. Christl, V. Connaughton, L. Conti, G. Cordero, G. Cotto, H. J. Crawford, R. Cremonini, S. Csorna, A. Cummings, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, M. Di Martino, A. Diaz Damian, T. Djemil, I. Dutan, A. Ebersoldt, T. Ebisuzaki, R. Engel, J. Eser, F. Fenu, S. Fernández-González, S. Ferrarese, M. Flamini, C. Fornaro, M. Fouka, A. Franceschi, S. Franchini, C. Fuglesang, T. Fujii, J. Fujimoto, M. Fukushima, P. Galeotti, E. García-Ortega, G. Garipov, E. Gascón, J. Genci, G. Giraudo, C. González Alvarado, P. Gorodetzky, R. Greg
    Astroparticle Physics 111 54 - 71 0927-6505 2019/09 [Refereed][Not invited]
     
    © 2018 The JEM-EUSO (Joint Experiment Missions for the Extreme Universe Space Observatory) program aims at developing Ultra-Violet (UV) fluorescence telescopes for efficient detections of Extensive Air Showers (EASs) induced by Ultra-High Energy Cosmic Rays (UHECRs) from satellite orbit. In order to demonstrate key technologies for JEM-EUSO, we constructed the EUSO-Balloon instrument that consists of a ∼1 m 2 refractive telescope with two Fresnel lenses and an array of multi-anode photo-multiplier tubes at the focus. Distinguishing it from the former balloon-borne experiments, EUSO-Balloon has the capabilities of single photon counting with a gate time of 2.3 µs and of imaging with a total of 2304 pixels. As a pathfinder mission, the instrument was launched for an 8 h stratospheric flight on a moonless night in August 2014 over Timmins, Canada. In this work, we analyze the count rates over ∼2.5 h intervals. The measurements are of diffuse light, e.g. of airglow emission, back-scattered from the Earth's atmosphere as well as artificial light sources. Count rates from such diffuse light are a background for EAS detections in future missions and relevant factor for the analysis of EAS events. We also obtain the geographical distribution of the count rates over a ∼780 km 2 area along the balloon trajectory. In developed areas, light sources such as the airport, mines, and factories are clearly identified. This demonstrates the correct location of signals that will be required for the EAS analysis in future missions. Although a precise determination of count rates is relevant for the existing instruments, the absolute intensity of diffuse light is deduced for the limited conditions by assuming spectra models and considering simulations of the instrument response. Based on the study of diffuse light by EUSO-Balloon, we also discuss the implications for coming pathfinders and future space-based UHECR observation missions.
  • K. Bandholnopparat, M. Sato, T. Adachi, T. Ushio, Y. Takahashi
    Journal of Atmospheric and Solar-Terrestrial Physics 189 87 - 97 1364-6826 2019/08 [Refereed][Not invited]
     
    © 2019 Elsevier Ltd We developed a new method to distinguish the lightning discharge type using lightning data obtained by JEM-GLIMS spaced-based mission and ground-based lightning network that are JLDN, NLDN, WWLLN, and GEON. As a first step, we selected 1057 lightning events detected by the JEM-GLIMS cameras (LSI) and spectrophotometers (PH) in 2014. Then, we compared the JEM-GLIMS optical data to the ground-based lightning data in order to check the simultaneous detection of JEM-GLIMS lightning events by the ground-based lightning networks, and finally we identified the discharge type of the JEM-GLIMS lightning events. We succeed in identifying 941 simultaneous lightning events and found that 582, 93, and 266 lightning events were IC, +CG, and -CG discharges, respectively. As a next step, we calculated intensity ratios between blue and red PH channels, i.e., 337nm/762 nm, 316nm/762 nm, 392nm/762 nm, 337nm/(599–900 nm), 316nm/(599–900 nm), and 392nm/(599–900 nm) for the 941 lightning events in order to specify the optical characteristics of IC, +CG, and -CG discharges. It is found that the PH intensity ratio of +CG discharges is the highest and that the PH intensity ratio of IC and -CG discharges is smaller than that of +CG discharge. We also found that the characteristics of the LSI intensity ratio are almost comparable to those of the PH intensity ratio. As the differences of the 337nm/762 nm, 337nm/(599–900 nm), and 392nm/(599–900 nm) ratio of IC, +CG, and -CG discharges are relatively large, these three ratios are a useful proxy for classifying the discharge types for additional 7349 lightning events detected by JEM-GLIMS in order to estimate the global ratio between IC and CG discharges (Z ratio).
  • Constraints on Venus lightning from Akatsuki's first three years in orbit
    Lorenz, Ralph D, M. Imai, Y. Takahashi, M. Sato, A. Yamazaki, T.M. Sato, T. Imamura, T. Satoh, M. Nakamura
    Geophys. Res. Lett. 46 7955 - 7961 2019/07 [Refereed][Not invited]
  • Gamma-ray glow preceding downward terrestrial gamma-ray flash
    Wada, Y, T. Enoto, Y. Nakamura, Y. Furuta, T. Yuasa, K. Nakazawa, T. Morimoto, M. Sato, T. Matsumoto, D. Yonetoku, T. Sawano, H. Sakai, M. Kamogawa, T. Ushio, K. Makishima, H. Tsuchiya
    Comm. Phys. 2 67  2019/06 [Refereed][Not invited]
  • Yukihiro Takahashi, Mitsuteru Sato, Masataka Imai, Ralph Lorenz, Yoav Yair, Karen Aplin, Georg Fischer, Masato Nakamura, Nobuaki Ishii, Takumi Abe, Takehiko Satoh, Takeshi Imamura, Chikako Hirose, Makoto Suzuki, George L. Hashimoto, Naru Hirata, Atsushi Yamazaki, Takao M. Sato, Manabu Yamada, Shin-ya Murakami, Yukio Yamamoto, Tetsuya Fukuhara, Kazunori Ogohara, Hiroki Ando, Ko-ichiro Sugiyama, Hiroki Kashimura, Shoko Ohtsuki
    Earth, Planets and Space 70 (1) 1880-5981 2018/12/01 [Refereed][Not invited]
     
    The existence of lightning discharges in the Venus atmosphere has been controversial for more than 30 years, with many positive and negative reports published. The lightning and airglow camera (LAC) onboard the Venus orbiter, Akatsuki, was designed to observe the light curve of possible flashes at a sufficiently high sampling rate to discriminate lightning from other sources and can thereby perform a more definitive search for optical emissions. Akatsuki arrived at Venus during December 2016, 5 years following its launch. The initial operations of LAC through November 2016 have included a progressive increase in the high voltage applied to the avalanche photodiode detector. LAC began lightning survey observations in December 2016. It was confirmed that the operational high voltage was achieved and that the triggering system functions correctly. LAC lightning search observations are planned to continue for several years.
  • Tomomi Narita, Egon Wanke, Mitsuteru Sato, Takeshi Sakanoi, Akiko Kumada, Masashi Kamogawa, Ishikawa Hirohiko, Shigemi Harada, Takao Kameda, Fuminori Tsuchiya, Eiji Kaneko
    34th International Conference on Lightning Protection, ICLP 2018 2018/10/23 [Refereed][Not invited]
     
    © 2018 IEEE. Blitzortung.org is a worldwide non-commercial low-cost community based Time of Arrival lightning detection and lightning location network. The aim of this project is to accomplish a low budget high accurate worldwide lightning location network based on a high number of receiver sites spaced close to each other, typically separated by 50 km 250km. The stations transmit their data to a central server, where the strike locations are computed by the arrival times of the signals. The station operators are volunteers who bought and assembled the hardware by themselves. We installed this sensor in more than 24 locations throughout Japan, for example Hokkaido, Tokyo, Okinawa, Ogasawara etc. This paper describes the outline of Blitzortung and the evaluation of the position accuracy.
  • Spectroscopic diagnostic of halos and elves detected from space-based photometers
    Pérez‐Invernón, F.J, A. Luque, F.J. Gordillo-Vázquez, M. Sato, T. Ushio, T. Adachi, A.B. Chen
    J. Geophys. Res. - Atmospheres 123 12917 - 12941 2018/10 [Refereed][Not invited]
  • Characteristics of thunderstorm structure and lightning activity causing negative and positive sprites
    Yang, J, N. Liu, M. Sato, G. Lu, Y. Wang, G. Feng
    J. Geophys. Res.: Atmospheres 123 (15) 8190 - 8207 2018/07 [Refereed][Not invited]
  • Start of lightning hunting by LAC / Akatsuki
    Takahashi, Y, M. Sato, M. Imai, R. Lorenz, Y. Yair, K. Aplin, G. Fischer, M. Nakamura, N. Ishii, T. Abe, T. Satoh, T. Imamura, C. Hirose, M. Suzuki, G. L. Hashimoto, N. Hitrata, A. Yamazaki, T. M. Sato, M. Yamada, S. Murakami, Y. Yamamoto, T. Fukuhara, K. Ogohara, H. Ando, K. Sugiyama, H. Kashimura, S. Ohtsuki
    Earth, Planets and Space 70:88 2018/05 [Refereed][Not invited]
  • Jing Yang, Mitsuteru Sato, Ningyu Liu, Gaopeng Lu, Yu Wang, Zhichao Wang
    Journal of Geophysical Research: Atmospheres 123 (2) 977 - 996 2169-8996 2018/01/27 [Refereed][Not invited]
     
    Gigantic jets (GJs) are mostly observed over summer tropical or tropical-like thunderstorms. This study reports observation of a GJ over a mesoscale convective system (MCS) in the midlatitude region in eastern China. The GJ is observed over a relatively weak radar reflectivity region ahead of the leading line, and the maximum radar echo top along the GJ azimuth was lower than the tropopause in the same region, significantly different from past studies that indicate summer GJs are usually associated with convective surges or overshooting tops. Also different from most of previous observations showing GJ-producing summer thunderstorms only produced GJ type of transient luminous events during their life cycles, two sprites were also captured in a time window of 15 min containing the GJ, indicating that the MCS provides favorable conditions not only for the GJ but also for the sprites. The balloon-borne soundings of the MCS show that there were large wind shears in the middle and upper levels of the thundercloud, which may have played important roles for the GJ production.
  • Daiki Tsurushima, Noriyasu Honma, Fuminori Tsuchiya, Mitsuteru Sato, Yukihiro Takahashi
    IEEJ Transactions on Power and Energy 138 (5) 339 - 345 1348-8147 2018 [Refereed][Not invited]
     
    ELF-band lightning electromagnetic pulses (ELF-LEMPs) have been used to retrieve lightning Charge Moment Change (CMC) and electric Current Waveform (CW). Since neither CMC nor CW can be measured by conventional Lightning Location System (LLS), it is advantageous to combine LLS and ELF measurements in order to monitor lightning geo-locations, CMC and CW simultaneously. To construct an accurate combined system of LLS and ELF measurements matching algorithms for associating lightning geo-locations and their corresponding ELF-LEMPs are important. This study developed three matching algorithms based on the time, the polarity and the direction of lightning discharges. Furthermore, we applied the newly developed algorithms to LLS and ELF measurements in Tohoku district and obtained a 30-70% Detection Efficiency (DE). The results also indicate that DE depends mainly on peak electric current (Ip). For example, DE exceeds 70% for lightning events with |Ip| ≥ 40 kA while DE drops below 70% for lower Ip events.
  • 超長波(VLF 帯)空電観測を用いた落雷位置標定システムの位置精度評価
    成田知巳, 佐藤光輝, 亀田貴雄, 坂野井健, 土屋史紀, 石井 勝, 熊田亜紀子, 鴨川 仁, 石川裕彦, 金子英治, 原田繁実, 工藤剛史, 茆原正昭, 皆川郁靖
    電気学会全国大会 7 (112) 175 - 176 2018 [Not refereed][Not invited]
  • Daisuke Kuroda, Masateru Ishiguro, Makoto Watanabe, Sunao Hasegawa, Tomohiko Sekiguchi, Hiroyuki Naito, Fumihiko Usui, Masataka Imai, Mitsuteru Sato, Kiyoshi Kuramoto
    Astronomy and Astrophysics 611 A31  1432-0746 2018 [Refereed][Not invited]
     
    We present a unique and significant polarimetric result regarding the near-Earth asteroid (152679) 1998 KU2, which has a very low geometric albedo. From our observations, we find that the linear polarization degrees of 1998 KU2 are 44.6 ± 0.5% in the RC band and 44.0 ± 0.6% in the V band at a solar phase angle of 81.0°. These values are the highest of any known airless body in the solar system (i.e., high-polarization comets, asteroids, and planetary satellites) at similar phase angles. This polarimetric observation is not only the first for primitive asteroids at large phase angles, but also for low-albedo (< 0.1) airless bodies. Based on spectroscopic similarities and polarimetric measurements of materials that have been sorted by size in previous studies, we conjecture that 1998 KU2 has a highly microporous regolith structure comprising nano-sized carbon grains on the surface.
  • Teruaki Enoto, Yuuki Wada, Yoshihiro Furuta, Kazuhiro Nakazawa, Takayuki Yuasa, Kazufumi Okuda, Kazuo Makishima, Mitsuteru Sato, Yousuke Sato, Toshio Nakano, Daigo Umemoto, Harufumi Tsuchiya
    NATURE 551 (7681) 481 - + 0028-0836 2017/11 [Refereed][Not invited]
     
    Lightning and thunderclouds are natural particle accelerators(1). Avalanches of relativistic runaway electrons, which develop in electric fields within thunderclouds(2,3), emit bremsstrahlung gamma-rays. These gamma-rays have been detected by ground-based observatories(4-9), by airborne detectors(10) and as terrestrial gamma-ray flashes from space(10-14). The energy of the gamma-rays is sufficiently high that they can trigger atmospheric photonuclear reactions(10,15-19) that produce neutrons and eventually positrons via beta(+) decay of the unstable radioactive isotopes, most notably N-13, which is generated via N-14 + gamma -> N-13 + n, where gamma denotes a photon and n a neutron. However, this reaction has hitherto not been observed conclusively, despite increasing observational evidence of neutrons(7,20,21) and positrons(10,22) that are presumably derived from such reactions. Here we report ground-based observations of neutron and positron signals after lightning. During a thunderstorm on 6 February 2017 in Japan, a gamma-ray flash with a duration of less than one millisecond was detected at our monitoring sites 0.5-1.7 kilometres away from the lightning. The subsequent gamma-ray afterglow subsided quickly, with an exponential decay constant of 40-60 milliseconds, and was followed by prolonged line emission at about 0.511 megaelectronvolts, which lasted for a minute. The observed decay time-scale and spectral cutoff at about 10 megaelectronvolts of the gamma-ray afterglow are well explained by de-excitation gamma-rays from nuclei excited by neutron capture. The centre energy of the prolonged line emission corresponds to electron-positron annihilation, providing conclusive evidence of positrons being produced after the lightning.
  • Polarimetric Study of Near-Earth Asteroid (1566) Icarus
    Ishiguro, M, D. Kuroda, M. Watanabe, Y. P. Bach, J. Kim, M. Lee, T. Sekiguchi, H. Naito, K. Ohtsuka, H. Hanayama, S. Hasegawa, F. Usui, S. Urakawa, M. Imai, M. Sato, K. Kuramoto
    The Astronomical Journal 154 180  2017/10 [Refereed][Not invited]
  • Tetsuya Fukuhara, Makoto Taguchi, Takeshi Imamura, Akane Hayashitani, Takeru Yamada, Masahiko Futaguchi, Toru Kouyama, Takao M. Sato, Mao Takamura, Naomoto Iwagami, Masato Nakamura, Makoto Suzuki, Munetaka Ueno, George L. Hashimoto, Mitsuteru Sato, Seiko Takagi, Atsushi Yamazaki, Manabu Yamada, Shin-ya Murakami, Yukio Yamamoto, Kazunori Ogohara, Hiroki Ando, Ko-ichiro Sugiyama, Hiroki Kashimura, Shoko Ohtsuki, Nobuaki Ishii, Takumi Abe, Takehiko Satoh, Chikako Hirose, Naru Hirata
    EARTH PLANETS AND SPACE 69 141  1880-5981 2017/10 [Refereed][Not invited]
     
    The Venus Climate Orbiter Akatsuki arrived at Venus in December 2015, and the Longwave Infrared Camera (LIR) onboard the spacecraft started making observations. LIR has acquired more than 8000 images during the first two Venusian years since orbit insertion without any serious faults. However, brightness temperature derived from LIR images contained an unexpected bias that related not to natural phenomena but to a thermal condition of the instrument. The bias could be partially eliminated by keeping the power supply unit for LIR always active, while the residual bias was simply correlated with the baffle temperature. Therefore, deep-space images were acquired at different baffle temperatures on orbit, and a reference table for eliminating the bias from images was prepared. In the corrected images, the brightness temperature was similar to 230 K at the center of the Venus disk, where the effect of limb darkening is negligible. The result is independent of the baffle temperature and consistent with the results of previous studies. Later, a laboratory experiment with the proto model of LIR showed that when the germanium (Ge) lens was heated, its actual temperature was slightly higher than the temperature measured by a thermal sensor attached to the lens holder. The experiment confirmed that transitory baffle heating accounted for the background bias found in the brightness temperature observed by LIR.
  • Mitsuteru Sato, Toru Adachi, Tomoo Ushio, Takeshi Morimoto, Masayuki Kikuchi, Hiroshi Kikuchi, Makoto Suzuki, Atsushi Yamazaki, Yukihiro Takahashi, Ryohei Ishida, Yuji Sakamoto, Kazuya Yoshida, Yasuhide Hobara
    TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES 28 (4) 545 - 561 1017-0839 2017/08 [Refereed][Not invited]
     
    The Global Lightning and Sprite Measurements on the Japanese Experiment Module (JEM-GLIMS) started continuous nadir observations of lightning and transient luminous events (TLEs) at the International Space Station (ISS) in November 2012 and completed the observations in August 2015. As JEM-GLIMS uses the nadir observation technique, the JEM-GLIMS optical instruments simultaneously measure both incomparably intense lightning emissions and weak sprite emissions. We adopted combined data analytical methods to distinguish between these two types of emissions: (1) a subtraction of the wideband LSI-1 image from the narrowband LSI-2 image, (2) a calculation of the intensity ratio between different photometer channels, and (3) an estimation of the charge moment change (CMC) of the suspected sprite-producing CG discharge. This report presents as a case study one sprite event detected at 19: 50: 40.30580 UT on 28 September 2013 and identified using the above analytical methods. From the results derived from detailed data analyses, we judged that the optical emission measured by LSI-2 is a sprite emission. We carried out the geometry conversion toward the LSI-1 and subtracted images and found that the sprite emission location shifts by 3.5 km from the peak lightning emission location, which agree with the previous reports. The detailed horizontal distributions of sprites and the relationship between the sprite location and the parent lightning location are quantitatively revealed for the first time.
  • Jing Yang, Gaopeng Lu, Ningyu Liu, Mitsuteru Sato, Guili Feng, Yu Wang, Jung-Kuang Chou
    TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES 28 (4) 609 - 624 1017-0839 2017/08 [Refereed][Not invited]
     
    Transient luminous event (TLEs) observations have been conducted in mainland China since 2007, with a number of TLEs documented. This study analyzed a very unusual and unique positive sprite event, that may be produced jointly by two distinct positive cloud-to-ground lightning flashes (+ CGs) occurring within a short time difference but with different locations separated by about 27 km. This observation is different from previous studies reporting that most of the sprites were triggered by a single + CG flash and its possible following continuous current. Detailed analysis on extremely low frequency (ELF) magnetic field shows that combined charge moment change (CMC) due to the two + CGs is smaller (similar to 1478 C km) than those of the parent CGs for the other two sprites (1582 and 2134 C km, respectively) recorded over the same thunderstorm. The vertical extension and brightness of the sprites correspond well with the CMC of their parent CGs, namely, the larger the CMC value the brighter the sprite, and the larger the CMC value the larger the vertical extension. Negative lightning flashes dominated during the thunderstorm life cycle. The three sprites occurred during a time window in which both negative and positive flashes were active. The three sprites occurred over the thunderstorm stratiform region.
  • M. Sato, T. Adachi, T. Ushio, T. Morimoto, M. Kikuchi, H. Kikuchi, M. Suzuki, A. Yamazaki, Y. Takahashi, R. Ishida, Y. Sakamoto, K. Yoshida, Y. Hobara
    Terrestrial, Atmospheric and Oceanic Sciences 28 (4) 545 - 561 1017-0839 2017/08 [Refereed][Not invited]
     
    © 2016 Terrestrial, Atmospheric and Oceanic Sciences (TAO). All rights reserved. The Global Lightning and Sprite Measurements on Japanese Experiment Module (JEM-GLIMS) started the continuous nadir observations of lightning and transient luminous events (TLEs) at the International Space Station (ISS) since November 2012 and finished the observations on August 2015. As JEM-GLIMS uses the nadir observation technique, the JEM-GLIMS optical instruments have to simultaneously measure both incomparably intense lightning emissions and weak sprite emissions. To distinguish them, we adopted combined data analytical methods: (1) a subtraction of the wideband LSI-1 image from the narrowband LSI-2 image, (2) a calculation of the intensity ratio between different photometer channels, and (3) an estimation of the charge moment change (CMC) of the suspected sprite-producing CG discharge. In this report, one sprite event detected at 19:50:40.30580 UT on September 28, 2013 and identified by above analytical methods is presented as a case study. From the results derived from detailed data analyses, we judged that the optical emission measured by LSI-2 is the sprite emission. We have carried out the geometry conversion toward the LSI-1 and subtracted images and found that the location of the sprite emission is shifter by 3.5 km from the location of the peak lightning emission, which well agree with the previous repots. Thus, the detailed horizontal distributions of sprites and the relation between the sprite location and the parent lightning location are quantitatively revealed for the first time.
  • Hiroko Miyahara, Chika Higuchi, Toshio Terasawa, Ryuho Kataoka, Mitsuteru Sato, Yukihiro Takahashi
    ANNALES GEOPHYSICAE 35 (3) 583 - 588 0992-7689 2017/04 [Refereed][Not invited]
     
    A signal of the 27-day solar rotational period is often observed in cloud and lightning activities over the globe. Here we provide evidence of the 27-day periodicity of lightning activity in Japan using daily observational records of lightning for AD1989-2015. The 27-day period is detected with 4.2 standard deviations, but only in wide-area lightning activity covering more than a 10(5) km(2). The 27-day signal is more prominent around the maxima of solar decadal cycles.
  • Tetsuya Fukuhara, Masahiko Futaguchi, George L. Hashimoto, Takeshi Horinouchi, Takeshi Imamura, Naomoto Iwagaimi, Toru Kouyama, Shin-ya Murakami, Masato Nakamura, Kazunori Ogohara, Mitsuteru Sato, Takao M. Sato, Makoto Suzuki, Makoto Taguchi, Seiko Takagi, Munetaka Ueno, Shigeto Watanabe, Manabu Yamada, Atsushi Yamazaki
    NATURE GEOSCIENCE 10 (2) 85 - + 1752-0894 2017/02 [Refereed][Not invited]
     
    The planet Venus is covered by thick clouds of sulfuric acid that move westwards because the entire upper atmosphere rotates much faster than the planet itself. At the cloud tops, about 65 km in altitude, small-scale features are predominantly carried by the background wind at speeds of approximately 100 ms(-1). In contrast, planetary-scale atmospheric features have been observed to move slightly faster or slower than the background wind, a phenomenon that has been interpreted to reflect the propagation of planetary-scale waves. Here we report the detection of an interhemispheric bow-shaped structure stretching 10,000 km across at the cloud-top level of Venus in middle infrared and ultraviolet images from the Japanese orbiter Akatsuki. Over several days of observation, the bow-shaped structure remained relatively fixed in position above the highland on the slowly rotating surface, despite the background atmospheric super rotation. We suggest that the bow-shaped structure is the result of an atmospheric gravity wave generated in the lower atmosphere by mountain topography that then propagated upwards. Numerical simulations provide preliminary support for this interpretation, but the formation and propagation of a mountain gravity wave remain difficult to reconcile with assumed near-surface conditions on Venus. We suggest that winds in the deep atmosphere may be spatially or temporally more variable than previously thought.
  • Broad-lined Supernova 2016coi with a Helium Envelope
    Yamanaka, M, T. Nakaoka, M. Tanaka, K. Maeda, S. Honda, H. Hanayama, T. Morokuma, M. Imai, K. Kinugasa, K.L. Murata, T. Nishimori, O. Hashimoto, H. Gima, K. Hosoya, A. Ito, M. Karita, M. Kawabata, K. Morihana, Y. Morikawa, K. Murakami, T. Nagayama, T. Ono, H. Onozato, Y. Sarugaku, M. Sato, D. Suzuki, J. Takahashi, M. Takayama, H. Yaguchi, H. Akitaya, Y. Asakura, K.S. Kawabata, D. Kuroda, D. Nogami, Y. Oasa, T. Omodaka, Y. Saito, K. Sekiguchi, N. Tominaga, M. Uemura, M. Watanabe
    The Astrophysical Journal 837 1  2017/02 [Refereed][Not invited]
  • Hiroshi Kikuchi, Mitsuteru Sato, Tomoo Ushio, Takeshi Morimoto, Masayuki Kikuchi, Atsushi Yamazaki, Makoto Suzuki, Ryohei Ishida, Yuji Sakamoto, Ting Wu, Zen Kawasaki
    GEOPHYSICAL RESEARCH LETTERS 44 (2) 1123 - 1131 0094-8276 2017/01 [Refereed][Not invited]
     
    Observations of optical lightning data with a photometer (PH4) at wavelengths of 599-900nm on the International Space Station were conducted simultaneously with observations of low-frequency (LF) electromagnetic waves with a ground-based LF lightning locating system. The relationship between the PH4 light curve and electromagnetic waveforms in the LF band was examined for 11 lightning events. The PH4 sensor detected a small optical change even for weak light emitted from lightning discharges in clouds, including preliminary breakdown. Particularly, return strokes, including subsequent return strokes, showed a clear relationship between radiated LF waves and optical waveforms. For negative return strokes, we found a clear correlation between the absolute optical intensity and peak current. The slope of the regression line is 9.7x10(-8)kAW(-1) with an intercept of 9.9kA.
  • Studies of dust and discharges around a Martian rover with onboard hazard analyses using electromagnetic and acoustic wave measurements
    Yamamoto, M, M. Sato, K. Ishisaka, Y. Takahashi, K. Ogohara, M. Kamogawa, H. Miyamoto
    Ttansactions of the Japan Society for Aeronatical and Space Sciences 14 (30) 41 - 45 2016/10 [Refereed][Not invited]
  • Takeshi Morimoto, Hiroshi Kikuchi, Mitsuteru Sato, Tomoo Ushio, Atsushi Yamazaki, Makoto Suzuki, Ryohei Ishida, Yuji Sakamoto, Kazuya Yoshida, Yasuhide Hobara, Takuki Sano, Takumi Abe, Zen-Ichiro Kawasaki
    EARTH PLANETS AND SPACE 68 145  1880-5981 2016/08 [Refereed][Not invited]
     
    The Global Lightning and sprIte MeasurementS (GLIMS) mission has been conducted at the Exposed Facility of Japanese Experiment Module (JEM-EF) of the International Space Station for more than 30 months. This paper focuses on an electromagnetic (EM) payload of JEM-GLIMS mission, the very high frequency (VHF) broadband digital InTer-Ferometer (VITF). The JEM-GLIMS mission is designed to conduct comprehensive observations with both EM and optical payloads for lightning activities and related transient luminous events. Its nominal operation continued from November 2012 to December 2014. The extended operation followed for eight months. Through the operation period, the VITF collected more than two million VHF EM waveforms in almost 18,700 datasets. The number of VITF observations synchronized with optical signal is 8049. Active VHF radiations are detected in about 70 % of optical observations without obvious regional or seasonal dependency. Estimations of the EM direction-of-arrival (DOA) are attempted using the broadband digital interferometry. Some results agree with the optical observations, even though DOA estimation is problematic because of a very short antenna baseline and multiple pulses over a short time period, namely burst-type EM waveforms. The world's first lightning observations by means of space-borne VHF interferometry are achieved in this mission. This paper summarizes VITF instruments, the recorded VHF EM signals, and the results of DOA estimations by means of digital interferometry as a preliminary report after termination of the mission.
  • Hiroshi Kikuchi, Takeshi Morimoto, Mitsuteru Sato, Tomoo Ushio, Masayuki Kikuchi, Atsushi Yamazaki, Makoto Suzuki, Ryohei Ishida, Yuji Sakamoto, Zen Kawasaki
    IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING 54 (7) 3868 - 3877 0196-2892 2016/07 [Refereed][Not invited]
     
    We report an initial investigation of the new location method of a very high frequency (VHF) radiation source, using signals recorded at the International Space Station. A VHF interferometer (VITF) has two VHF sensors. Locating lightning with VHF bands is useful to locate the position of the charge distribution in the thunderstorm. The location method of a radio source proposed used two direction-of-arrival estimation techniques. One is the interferometric technique, and another is based on the ionospheric propagation delay measurement of received signals. The combination of the two techniques provides two angular positions of the radiation source. When an altitude of a radiation source is assumed, we can determine two possible positions. One of the two positions was associated with the radiation source, while the other was not. In this paper, we compared the position of lightning and sprite imager (LSI) data, which are simultaneously captured during a lightning emission, with the locating position near the emission. The data set of the VITF within 100 ms of the optical lightning emission captured with the LSI was used. The temporally simultaneous event seems to be associated with the same lightning event. The estimated radiation positions were spatially in close agreement with the optical lightning positions captured with LSI, under nighttime ionosphere conditions. From statistical analysis, the spatial difference of the standard deviation changed from 15.3 to 30.8 km depending on the installation direction of the VHF sensors. The usefulness and limitations of the method are also discussed.
  • Toru Adachi, Mitsuteru Sato, Tomoo Ushio, Atsushi Yamazaki, Makoto Suzuki, Masayuki Kikuchi, Yukihiro Takahashi, Umran S. Inan, Ivan Linscott, Yasuhide Hobara, Harald U. Frey, Stephen B. Mende, Alfred B. Chen, Rue-Ron Hsu, Kenichi Kusunoki
    JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS 145 85 - 97 1364-6826 2016/07 [Refereed][Not invited]
     
    We propose a new technique to identify the occurrence of lightning and transient luminous events (TLEs) using multicolor photometric data obtained by space borne nadir measurements. We estimate the spectral characteristics of lightning and TLEs by converting the optical data obtained by the ISUAL limb experiment to the GUMS nadir geometry. We find that the estimated spectral shapes of TLE-accompanied lightning are clearly different from those of pure lightning. The obtained results show that (1) the intensity of FIN signals and (2) the ratio of 337/red (609-753 nm) spectral irradiance are useful to identify the occurrence of TLEs. The occurrence probabilities of TLEs are 10%, 40%, 80%, in the case of lightning events having the 337/red spectral irradiance ratio of 0.95, 2.95, 14.79, respectively. By using the 60% criterion of the 337/red ratio and the existence of FUN emissions, we classify the 1039 GLIMS-observed lightning events into 828 pure lightning and 211 TLE-accompanied lightning. Since the GUMS trigger level is adjusted to observe extremely-bright events, the occurrence probability of TLEs obtained here most probably reflects the characteristics of energetic lightning. The estimated global map is consistent with previously determined distributions: the highest activities of lightning and TLEs are found over the North/South American continents, African continent, and Asian maritime regions. While the absolute occurrence number of pure lightning and TLE-accompanied lightning are found to maximize in the equatorial region, the occurrence probability of TLEs possibly increase somewhat in the mid-latitude region. Since the occurrence probabilities of TLEs are higher over the ocean than over land, it is likely that the GUMS-observed TLEs are due primarily to elves which tends to occur more frequently over the ocean. (C) 2016 Elsevier Ltd. All rights reserved.
  • M. Sato, M. Mihara, T. Adachi, T. Ushio, T. Morimoto, M. Kikuchi, H. Kikuchi, M. Suzuki, A. Yamazaki, Y. Takahashi, U. Inan, I. Linscott, R. Ishida, Y. Sakamoto, K. Yoshida, Y. Hobara
    JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES 121 (7) 3171 - 3194 2169-897X 2016/04 [Refereed][Not invited]
     
    Global Lightning and Sprite Measurements on Japanese Experiment Module (JEM-GLIMS) started the nadir observations of lightning discharges and transient luminous events (TLEs) from the International Space Station (ISS) since November 2012. In the nadir observations, JEM-GLIMS optical instruments have to simultaneously detect incomparably intense lightning emissions and weak TLE emissions. To distinguish TLEs, especially sprite events, from lightning events, combined data analytical methods are adopted: (1) a subtraction of the wideband camera image from the narrowband camera image, (2) a calculation of the intensity ratio between different photometer channels, and (3) an estimation of the polarization and charge moment changes for the TLE-producing lightning discharges. We succeeded in identifying numbers of sprite events using the combined analytical methods, and here we report three sprite events detected by JEM-GLIMS as a case study. In the subtracted images, sprite emissions are located over the area of the sprite-producing lightning emissions. However, these sprites and sprite-producing lightning discharges did not occur at the nadir point of the ISS. For this reason, the geometry conversion of the sprite and sprite-producing lightning emissions as observed from the point just over the sprite-producing lightning discharges is performed. In the geometry-converted images, the locations of the sprite emissions are clearly displaced by 8-20km from the peak positions of the sprite-producing lightning emissions. Thus, the first quantitative spatial distributions of sprites and sprite-producing lightning discharges from the JEM-GLIMS nadir observations are revealed.
  • M. Sato, M. Mihara, T. Adachi, T. Ushio, T. Morimoto, M. Kikuchi, H. Kikuchi, M. Suzuki, A. Yamazaki, Y. Takahashi, U. Inan, I. Linscott, R. Ishida, Y. Sakamoto, K. Yoshida, Y. Hobara
    Journal of Geophysical Research 121 (7) 3171 - 3194 0148-0227 2016 [Refereed][Not invited]
     
    © 2016. American Geophysical Union. All Rights Reserved. Global Lightning and Sprite Measurements on Japanese Experiment Module (JEM-GLIMS) started the nadir observations of lightning discharges and transient luminous events (TLEs) from the International Space Station (ISS) since November 2012. In the nadir observations, JEM-GLIMS optical instruments have to simultaneously detect incomparably intense lightning emissions and weak TLE emissions. To distinguish TLEs, especially sprite events, from lightning events, combined data analytical methods are adopted: (1) a subtraction of the wideband camera image from the narrowband camera image, (2) a calculation of the intensity ratio between different photometer channels, and (3) an estimation of the polarization and charge moment changes for the TLE-producing lightning discharges. We succeeded in identifying numbers of sprite events using the combined analytical methods, and here we report three sprite events detected by JEM-GLIMS as a case study. In the subtracted images, sprite emissions are located over the area of the sprite-producing lightning emissions. However, these sprites and sprite-producing lightning discharges did not occur at the nadir point of the ISS. For this reason, the geometry conversion of the sprite and sprite-producing lightning emissions as observed from the point just over the sprite-producing lightning discharges is performed. In the geometry-converted images, the locations of the sprite emissions are clearly displaced by 8-20 km from the peak positions of the sprite-producing lightning emissions. Thus, the first quantitative spatial distributions of sprites and sprite-producing lightning discharges from the JEM-GLIMS nadir observations are revealed.
  • Chihau Shimizu, Mitsuteni Sato, Yasuji Hongo, Fiiniiiiori Tsuchiya, Yukihiro Takahashi
    IEEJ Transactions on Fundamentals and Materials 136 (5) 252 - 258 1347-5533 2016 [Refereed][Not invited]
     
    Recently, it was shown that the shape of lightning-generated induction magnetic field waveforms in the ELF frequency range is well comparable to that of lightning current waveforms. Therefore, charge amounts of any lightning discharges occurring within the area where the induction magnetic fields are measured can be easily estimated from ELF waveforms by quantitatively evaluating the relation between ELF waveforms and the current waveforms. In this study, we analyzed lightning current waveforms measured by a Rogowski coil installed at Mt. Ogkami and ELF waveforms measured at Onagawa observatory. Based on the quantitative comparison between the ELF waveforms and the current waveforms, empirical equations that enable us to directly convert from the magnetic field intensities into the current intensities and charge amount were obtained. Furthermore, using ELF waveform data obtained at Kuju station in Kyushu and the Japan Lightning Detection Network (JLDN) lightning data, peak current values and charge amounts for the lightning discharges occurring when severe downbursts occurred in the Kanto Plain were estimated by applying the empirical equations. Then, we newly found a clear feature showing that the time variation of charge amounts drastically changed just before the downburst onset.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 (1) 315 - 326 0922-6435 2015/11 [Refereed][Not invited]
     
    Space-based detectors for the study of extreme energy cosmic rays (EECR) are being prepared as a promising new method for detecting highest energy cosmic rays. A pioneering space device - the "tracking ultraviolet set-up" (TUS) - is in the last stage of its construction and testing. The TUS detector will collect preliminary data on EECR in the conditions of a space environment, which will be extremely useful for planning the major JEM-EUSO detector operation.
  • The JEM-EUSO Collaboration, J. H. Adams, S. Ahmad, J. N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Błȩcki, S. Blin-Bondil, J. Blümer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J. N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellinic, C. Catalano, G. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell’Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernández-Gómez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. González Alvarado, P. Gorodetzky, F. Guarino, A. Guzmán, Y. Hachisu, B. Harlov, A. Haungs, J. Hernández Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgrò, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, J. S. Kim, S. W. Kim, S. W. Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. López, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Ríos, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano Murakami, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleański, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prévôt, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodríguez, M. D. Rodríguez Frías, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczyński, M. D. Sabau, G. Sáez-Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sánchez, A. Santangelo, L. Santiago Crúz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Oziȩbło, H. H. Silva López, J. Sledd, K. Słomińska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdés-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villaseñor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Włodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    Experimental Astronomy 40 (1) 301 - 314 1572-9508 2015/11/01 [Refereed][Not invited]
     
    We are conducting tests of optical and electronics components of JEMEUSO at the Telescope Array site in Utah with a ground-based “EUSO-TA” detector. The tests will include an engineering validation of the detector, cross-calibration of EUSO-TA with the TA fluorescence detector and observations of air shower events. Also, the proximity of the TA’s Electron Light Source will allow for convenient use of this calibration device. In this paper, we report initial results obtained with the EUSO-TA telescope.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchari, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itowen, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wl Odarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 (1) 281 - 299 0922-6435 2015/11 [Refereed][Not invited]
     
    EUSO-Balloon is a pathfinder for JEM-EUSO, the Extreme Universe Space Observatory which is to be hosted on-board the International Space Station. As JEM-EUSO is designed to observe Ultra-High Energy Cosmic Rays (UHECR)-induced Extensive Air Showers (EAS) by detecting their ultraviolet light tracks "from above", EUSO-Balloon is a nadir-pointing UV telescope too. With its Fresnel Optics and Photo-Detector Module, the instrument monitors a 50 km(2) ground surface area in a wavelength band of 290-430 nm, collecting series of images at a rate of 400,000 frames/sec. The objectives of the balloon demonstrator are threefold: a) perform a full end-to-end test of a JEM-EUSO prototype consisting of all the main subsystems of the space experiment, b) measure the effective terrestrial UV background, with a spatial and temporal resolution relevant for JEM-EUSO. c) detect tracks of ultraviolet light from near space for the first time. The latter is a milestone in the development of UHECR science, paving the way for any future space-based UHECR observatory. On August 25, 2014, EUSO-Balloon was launched from Timmins Stratospheric Balloon Base (Ontario, Canada) by the balloon division of the French Space Agency CNES. From a float altitude of 38 km, the instrument operated during the entire astronomical night, observing UV-light from a variety of ground-covers and from hundreds of simulated EASs, produced by flashers and a laser during a two-hour helicopter under-flight.
  • The JEM-EUSO Collaboration, J. H. Adams, S. Ahmad, J. N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Błȩcki, S. Blin-Bondil, J. Blümer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J. N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellinic, C. Catalano, G. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell’Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernández-Gómez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. González Alvarado, P. Gorodetzky, F. Guarino, A. Guzmán, Y. Hachisu, B. Harlov, A. Haungs, J. Hernández Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgrò, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, J. S. Kim, S. W. Kim, S. W. Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. López, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Ríos, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano Murakami, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleański, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prévôt, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodríguez, M. D. Rodríguez Frías, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczyński, M. D. Sabau, G. Sáez-Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sánchez, A. Santangelo, L. Santiago Crúz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Oziȩbło, H. H. Silva López, J. Sledd, K. Słomińska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdés-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villaseñor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Włodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    Experimental Astronomy 40 (1) 253 - 279 1572-9508 2015/11/01 [Refereed][Not invited]
     
    Meteor and fireball observations are key to the derivation of both the inventory and physical characterization of small solar system bodies orbiting in the vicinity of the Earth. For several decades, observation of these phenomena has only been possible via ground-based instruments. The proposed JEM-EUSO mission has the potential to become the first operational space-based platform to share this capability. In comparison to the observation of extremely energetic cosmic ray events, which is the primary objective of JEM-EUSO, meteor phenomena are very slow, since their typical speeds are of the order of a few tens of km/sec (whereas cosmic rays travel at light speed). The observing strategy developed to detect meteors may also be applied to the detection of nuclearites, which have higher velocities, a wider range of possible trajectories, but move well below the speed of light and can therefore be considered as slow events for JEM-EUSO. The possible detection of nuclearites greatly enhances the scientific rationale behind the JEM-EUSO mission.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galiciaga, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 (1) 239 - 251 0922-6435 2015/11 [Refereed][Not invited]
     
    The main goal of the JEM-EUSO experiment is the study of Ultra High Energy Cosmic Rays (UHECR, 10(19)-10(21) e V), but the method which will be used (detection of the secondary light emissions induced by cosmic rays in the atmosphere) allows to study other luminous phenomena. The UHECRs will be detected through the measurement of the emission in the range between 290 and 430 m, where some part of Transient Luminous Events (TLEs) emission also appears. This work discusses the possibility of using the JEM-EUSO Telescope to get new scientific results on TLEs. The high time resolution of this instrument allows to observe the evolution of TLEs with great precision just at the moment of their origin. The paper consists of four parts: review of the present knowledge on the TLE, presentation of the results of the simulations of the TLE images in the JEM-EUSO telescope, results of the Russian experiment Tatiana-2 and discussion of the possible progress achievable in this field with JEM-EUSO as well as possible cooperation with other space projects devoted to the study of TLE - TARANIS and ASIM. In atmospheric physics, the study of TLEs became one of the main physical subjects of interest after their discovery in 1989. In the years 1992 - 1994 detection was performed from satellite, aircraft and space shuttle and recently from the International Space Station. These events have short duration (milliseconds) and small scales (km to tens of km) and appear at altitudes 50 - 100 km. Their nature is still not clear and each new experimental data can be useful for a better understanding of these mysterious phenomena.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgr'o, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, A. D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 (1) 235 - 237 0922-6435 2015/11 [Refereed][Not invited]
  • A. D. Supanitsky, G. Medina-Tanco, A. Guzman
    EXPERIMENTAL ASTRONOMY 40 (1) 215 - 233 0922-6435 2015/11 [Refereed][Not invited]
     
    Ultra high energy photons and neutrinos are carriers of very important astrophysical information. They may be produced at the sites of cosmic ray acceleration or during the propagation of the cosmic rays in the intergalactic medium. In contrast to charged cosmic rays, photon and neutrino arrival directions point to the production site because they are not deflected by the magnetic fields of the Galaxy or the intergalactic medium. In this work we study the characteristics of the longitudinal development of showers initiated by photons and neutrinos at the highest energies. These studies are relevant for development of techniques for neutrino and photon identification by the JEM-EUSO telescope. In particular, we study the possibility of observing the multi-peak structure of very deep horizontal neutrino showers with JEM-EUSO. We also discuss the possibility to determine the flavor content of the incident neutrino flux by taking advantage of the different characteristics of the longitudinal profiles generated by different type of neutrinos. This is of grate importance for the study of the fundamental properties of neutrinos at the highest energies. Regarding photons, we discuss the detectability of the cosmogenic component by JEM-EUSO and also estimate the expected upper limits on the photon fraction which can be obtained from the future JEM-EUSO data for the case in which there are no photons in the samples.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de Los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov
    EXPERIMENTAL ASTRONOMY 40 (1) 183 - 214 0922-6435 2015/11 [Refereed][Not invited]
     
    The Extreme Universe Space Observatory (EUSO) on-board the Japanese Experimental Module (JEM) of the International Space Station aims at the detection of ultra high energy cosmic rays from space. The mission consists of a UV telescope which will detect the fluorescence light emitted by cosmic ray showers in the atmosphere. The mission, currently developed by a large international collaboration, is designed to be launched within this decade. In this article, we present the reconstruction of the energy of the observed events and we also address the X (max) reconstruction. After discussing the algorithms developed for the energy and X (max) reconstruction, we present several estimates of the energy resolution, as a function of the incident angle, and energy of the event. Similarly, estimates of the X (max) resolution for various conditions are presented.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csoma, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fern'andez-G'omez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonz'alez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hern'andez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgr'o, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. L'opez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los R'ios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orlea'nski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Pr'evot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodr'iguez, M. D. Rodr'iguez Fr'ias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczy'nski, M. D. Sabau, G. S'aez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. S'anchez, A. Santangelo, L. Santiago Cr'uz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva L'opez, J. Sledd, K. Slomi'nska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Vald'es-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov
    EXPERIMENTAL ASTRONOMY 40 (1) 179 - 181 0922-6435 2015/11 [Refereed][Not invited]
  • The JEM-EUSO Collaboration, J. H. Adams, S. Ahmad, J. N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Błȩcki, S. Blin-Bondil, J. Blümer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J. N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellinic, C. Catalano, G. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell’Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernández-Gómez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. González Alvarado, P. Gorodetzky, F. Guarino, A. Guzmán, Y. Hachisu, B. Harlov, A. Haungs, J. Hernández Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgrò, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, J. S. Kim, S. W. Kim, S. W. Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. López, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Ríos, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano Murakami, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleański, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prévôt, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodríguez, M. D. Rodríguez Frías, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczyński, M. D. Sabau, G. Sáez-Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sánchez, A. Santangelo, L. Santiago Crúz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Oziȩbło, H. H. Silva López, J. Sledd, K. Słomińska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdés-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villaseñor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Włodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    Experimental Astronomy 40 (1) 153 - 177 1572-9508 2015/11/01 [Refereed][Not invited]
     
    Mounted on the International Space Station(ISS), the Extreme Universe Space Observatory, on-board the Japanese Experimental Module (JEM-EUSO), relies on the well established fluorescence technique to observe Extensive Air Showers (EAS) developing in the earth’s atmosphere. Focusing on the detection of Ultra High Energy Cosmic Rays (UHECR) in the decade of 1020eV, JEM-EUSO will face new challenges by applying this technique from space. The EUSO Simulation and Analysis Framework (ESAF) has been developed in this context to provide a full end-to-end simulation frame, and assess the overall performance of the detector. Within ESAF, angular reconstruction can be separated into two conceptually different steps. The first step is pattern recognition, or filtering, of the signal to separate it from the background. The second step is to perform different types of fitting in order to search for the relevant geometrical parameters that best describe the previously selected signal. In this paper, we discuss some of the techniques we have implemented in ESAF to perform the geometrical reconstruction of EAS seen by JEM-EUSO. We also conduct thorough tests to assess the performances of these techniques in conditions which are relevant to the scope of the JEM-EUSO mission. We conclude by showing the expected angular resolution in the energy range that JEM-EUSO is expected to observe.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornarodo, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircakja, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 (1) 135 - 152 0922-6435 2015/11 [Refereed][Not invited]
     
    The JEM-EUSO (Extreme Universe Space Observatory on-board the Japanese Experiment Module) mission will conduct extensive air shower (EAS) observations on the International Space Station (ISS). Following the ISS orbit, JEM-EUSO will experience continuous changes in the atmospheric conditions, including cloud presence. The influence of clouds on space-based observation is, therefore, an important topic to investigate from both EAS property and cloud climatology points of view. In the present work, the impact of clouds on the apparent profile of EAS is demonstrated through the simulation studies, taking into account the JEM-EUSO instrument and properties of the clouds. These results show a dependence on the cloud-top altitude and optical depth of the cloud. The analyses of satellite measurements on the cloud distribution indicate that more than 60 % of the cases allow for conventional EAS observation, and an additional similar to 20 % with reduced quality. The combination of the relevant factors results in an effective trigger aperture of EAS observation similar to 72 %, compared to the one in the clear atmosphere condition.
  • M. Bertaina, P. Bobik, F. Fenu, K. Shinozaki
    EXPERIMENTAL ASTRONOMY 40 (1) 117 - 134 0922-6435 2015/11 [Refereed][Not invited]
     
    Designed as the first mission to explore the ultra-high energy universe from space, JEM-EUSO observes the Earth's atmosphere at night to record the ultraviolet tracks generated by the extensive air showers. We present the expected geometrical aperture and annual exposure in the nadir and tilt modes for ultra-high energy cosmic rays observation as a function of the altitude of the International Space Station.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. de Donato, C. de la Taille, C. de Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 (1) 91 - 116 0922-6435 2015/11 [Refereed][Not invited]
     
    The JEM-EUSO telescope will be, after calibration, a very accurate instrument which yields the number of received photons from the number of measured photo-electrons. The project is in phase A (demonstration of the concept) including already operating prototype instruments, i.e. many parts of the instrument have been constructed and tested. Calibration is a crucial part of the instrument and its use. The focal surface (FS) of the JEM-EUSO telescope will consist of about 5000 photo-multiplier tubes (PMTs), which have to be well calibrated to reach the required accuracy in reconstructing the air-shower parameters. The optics system consists of 3 plastic Fresnel (double-sided) lenses of 2.5 m diameter. The aim of the calibration system is to measure the efficiencies (transmittances) of the optics and absolute efficiencies of the entire focal surface detector. The system consists of 3 main components: (i) Pre-flight calibration devices on ground, where the efficiency and gain of the PMTs will be measured absolutely and also the transmittance of the optics will be. (ii) On-board relative calibration system applying two methods: a) operating during the day when the JEM-EUSO lid will be closed with small light sources on board. b) operating during the night, together with data taking: the monitoring of the background rate over identical sites. (iii) Absolute in-flight calibration, again, applying two methods: a) measurement of the moon light, reflected on high altitude, high albedo clouds. b) measurements of calibrated flashes and tracks produced by the Global Light System (GLS). Some details of each calibration method will be described in this paper.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashini, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotovi, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 (1) 61 - 89 0922-6435 2015/11 [Refereed][Not invited]
     
    The Extreme Universe Space Observatory on the Japanese Experiment Module (JEM-EUSO) on board the International Space Station (ISS) is the first space-based mission worldwide in the field of Ultra High-Energy Cosmic Rays (UHECR). For UHECR experiments, the atmosphere is not only the showering calorimeter for the primary cosmic rays, it is an essential part of the readout system, as well. Moreover, the atmosphere must be calibrated and has to be considered as input for the analysis of the fluorescence signals. Therefore, the JEM-EUSO Space Observatory is implementing an Atmospheric Monitoring System (AMS) that will include an IR-Camera and a LIDAR. The AMS Infrared Camera is an infrared, wide FoV, imaging system designed to provide the cloud coverage along the JEM-EUSO track and the cloud top height to properly achieve the UHECR reconstruction in cloudy conditions. In this paper, an updated preliminary design status, the results from the calibration tests of the first prototype, the simulation of the instrument, and preliminary cloud top height retrieval algorithms are presented.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 (1) 45 - 60 0922-6435 2015/11 [Refereed][Not invited]
     
    The JEM-EUSO telescope will detect Ultra-High Energy Cosmic Rays (UHECRs) from space, detecting the UV Fluorescence Light produced by Extensive Air Showers (EAS) induced by the interaction of the cosmic rays with the earth's atmosphere. The capability to reconstruct the properties of the primary cosmic ray depends on the accurate measurement of the atmospheric conditions in the region of EAS development. The Atmospheric Monitoring (AM) system of JEM-EUSO will host a LIDAR, operating in the UV band, and an Infrared camera to monitor the cloud cover in the JEM-EUSO Field of View, in order to be sensitive to clouds with an optical depth tau a parts per thousand yen 0.15 and to measure the cloud top altitude with an accuracy of 500 m and an altitude resolution of 500 m.
  • The JEM-EUSO Collaboration, J. H. Adams, S. Ahmad, J. N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Błȩcki, S. Blin-Bondil, J. Blümer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J. N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellinic, C. Catalano, G. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell’Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernández-Gómez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. González Alvarado, P. Gorodetzky, F. Guarino, A. Guzmán, Y. Hachisu, B. Harlov, A. Haungs, J. Hernández Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgrò, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, J. S. Kim, S. W. Kim, S. W. Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. López, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Ríos, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano Murakami, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleański, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prévôt, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodríguez, M. D. Rodríguez Frías, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczyński, M. D. Sabau, G. Sáez-Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sánchez, A. Santangelo, L. Santiago Crúz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Oziȩbło, H. H. Silva López, J. Sledd, K. Słomińska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdés-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villaseñor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Włodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    Experimental Astronomy 40 (1) 19 - 44 1572-9508 2015/11/01 [Refereed][Not invited]
     
    In this paper we describe the main characteristics of the JEM-EUSO instrument. The Extreme Universe Space Observatory on the Japanese Experiment Module (JEM-EUSO) of the International Space Station (ISS) will observe Ultra High-Energy Cosmic Rays (UHECR) from space. It will detect UV-light of Extensive Air Showers (EAS) produced by UHECRs traversing the Earth’s atmosphere. For each event, the detector will determine the energy, arrival direction and the type of the primary particle. The advantage of a space-borne detector resides in the large field of view, using a target volume of about 1012 tons of atmosphere, far greater than what is achievable from ground. Another advantage is a nearly uniform sampling of the whole celestial sphere. The corresponding increase in statistics will help to clarify the origin and sources of UHECRs and characterize the environment traversed during their production and propagation. JEM-EUSO is a 1.1 ton refractor telescope using an optics of 2.5 m diameter Fresnel lenses to focus the UV-light from EAS on a focal surface composed of about 5,000 multi-anode photomultipliers, for a total of ≃3⋅105 channels. A multi-layer parallel architecture handles front-end acquisition, selecting and storing valid triggers. Each processing level filters the events with increasingly complex algorithms using FPGAs and DSPs to reject spurious events and reduce the data rate to a value compatible with downlink constraints.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. de Donato, C. de la Taille, C. de Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de Los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 (1) 3 - 17 0922-6435 2015/11 [Refereed][Not invited]
     
    The Extreme Universe Space Observatory on board the Japanese Experiment Module of the International Space Station, JEM-EUSO, is being designed to search from space ultra-high energy cosmic rays. These are charged particles with energies from a few 10(19) eV to beyond 10(20) eV, at the very end of the known cosmic ray energy spectrum. JEM-EUSO will also search for extreme energy neutrinos, photons, and exotic particles, providing a unique opportunity to explore largely unknown phenomena in our Universe. The mission, principally based on a wide field of view (60 degrees) near-UV telescope with a diameter of similar to 2.5 m, will monitor the earth's atmosphere at night, pioneering the observation from space of the ultraviolet tracks (290-430 nm) associated with giant extensive air showers produced by ultra-high energy primaries propagating in the earth's atmosphere. Observing from an orbital altitude of similar to 400 km, the mission is expected to reach an instantaneous geometrical aperture of A (g e o) a parts per thousand yen 2 x 10(5) km(2) sr with an estimated duty cycle of similar to 20 %. Such a geometrical aperture allows unprecedented exposures, significantly larger than can be obtained with ground-based experiments. In this paper we briefly review the history of space-based search for ultra-high energy cosmic rays. We then introduce the special issue of Experimental Astronomy devoted to the various aspects of such a challenging enterprise. We also summarise the activities of the on-going JEM-EUSO program.
  • M. Sato, T. Ushio, T. Morimoto, M. Kikuchi, H. Kikuchi, T. Adachi, M. Suzuki, A. Yamazaki, Y. Takahashi, U. Inan, I. Linscott, R. Ishida, Y. Sakamoto, K. Yoshida, Y. Hobara, T. Sano, T. Abe, M. Nakamura, H. Oda, Z. -I. Kawasaki
    JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES 120 (9) 3822 - 3851 2169-897X 2015/05 [Refereed][Not invited]
     
    Global Lightning and Sprite Measurements on Japanese Experiment Module (JEM-GLIMS) is a space mission to conduct the nadir observations of lightning discharges and transient luminous events (TLEs). The main objectives of this mission are to identify the horizontal distribution of TLEs and to solve the occurrence conditions determining the spatial distribution. JEM-GLIMS was successfully launched and started continuous nadir observations in 2012. The global distribution of the detected lightning events shows that most of the events occurred over continental regions in the local summer hemisphere. In some events, strong far-ultraviolet emissions have been simultaneously detected with N-2 1P and 2P emissions by the spectrophotometers, which strongly suggest the occurrence of TLEs. Especially, in some of these events, no significant optical emission was measured by the narrowband filter camera, which suggests the occurrence of elves, not sprites. The VLF receiver also succeeded in detecting lightning whistlers, which show clear falling-tone frequency dispersion. Based on the optical data, the time delay from the detected lightning emission to the whistlers was identified as approximate to 10ms, which can be reasonably explained by the wave propagation with the group velocity of whistlers. The VHF interferometer conducted the spaceborne interferometric observations and succeeded in detecting VHF pulses. We observed that the VHF pulses are likely to be excited by the lightning discharge possibly related with in-cloud discharges and measured with the JEM-GLIMS optical instruments. Thus, JEM-GLIMS provides the first full set of optical and electromagnetic data of lightning and TLEs obtained by nadir observations from space.
  • M. Sato, T. Ushio, T. Morimoto, M. Kikuchi, H. Kikuchi, T. Adachi, M. Suzuki, A. Yamazaki, Y. Takahashi, U. Inan, I. Linscott, R. Ishida, Y. Sakamoto, K. Yoshida, Y. Hobara, T. Sano, T. Abe, M. Nakamura, H. Oda, Z. I. Kawasaki
    Journal of Geophysical Research 120 (9) 3822 - 3851 0148-0227 2015 [Refereed][Not invited]
     
    © 2015. American Geophysical Union. All Rights Reserved. Global Lightning and Sprite Measurements on Japanese Experiment Module (JEM-GLIMS) is a space mission to conduct the nadir observations of lightning discharges and transient luminous events (TLEs). The main objectives of this mission are to identify the horizontal distribution of TLEs and to solve the occurrence conditions determining the spatial distribution. JEM-GLIMS was successfully launched and started continuous nadir observations in 2012. The global distribution of the detected lightning events shows that most of the events occurred over continental regions in the local summer hemisphere. In some events, strong far-ultraviolet emissions have been simultaneously detected with N2 1P and 2P emissions by the spectrophotometers, which strongly suggest the occurrence of TLEs. Especially, in some of these events, no significant optical emission was measured by the narrowband filter camera, which suggests the occurrence of elves, not sprites. The VLF receiver also succeeded in detecting lightning whistlers, which show clear falling-tone frequency dispersion. Based on the optical data, the time delay from the detected lightning emission to the whistlers was identified as ~10 ms, which can be reasonably explained by the wave propagation with the group velocity of whistlers. The VHF interferometer conducted the spaceborne interferometric observations and succeeded in detecting VHF pulses. We observed that the VHF pulses are likely to be excited by the lightning discharge possibly related with in-cloud discharges and measured with the JEM-GLIMS optical instruments. Thus, JEM-GLIMS provides the first full set of optical and electromagnetic data of lightning and TLEs obtained by nadir observations from space.
  • Hiroshi Kikuchi, Tomoo Ushio, Mitsuteru Sato, Takeshi Morimoto, Atsushi Yamazaki, Makoto Suzuki
    IEEE International Symposium on Electromagnetic Compatibility 2014-December 398 - 401 1077-4076 2014/12/23 [Refereed][Not invited]
     
    © 2014 The Institute of Electronics, Information and Communication Engineer. Since 2012, the global lightning and sprite measurements (GLIMS) mission has been conducted on the exposed facility of Japanese experiment module (JEM-EF) of the international space station (ISS). In this mission, the VHF broadband digital interferometer (VITF) attached on JEM-EF is designed to estimate the direction of arrival of electromagnetic waves. The VITF has the bandwidth from 70 MHz to 100 MHz. The electromagnetic radiations from lightning discharges received by two antennas are digitized by the 2-channel AD converter. We introduce the outline of the mission and the VITF. The initial observational results with the VITF of the GLIMS mission are presented. The comparison of the results of arrival direction estimation of the VITF with optical observations using two methods which are an interferometry technic and the group delay characteristic of EM waves. The results agree with the position of the lightning emission captured by the LSI.
  • Hiroshi Kikuchi, Takeshi Morimoto, Tomoo Ushio, Mitsuteru Sato, Atsushi Yamazaki, Makoto Suzuki
    International Conference on Atmospheric Electricity, ICAE 2014 2014 [Refereed][Not invited]
     
    © International Conference on Atmospheric Electricity, ICAE 2014 We has been conducted the lightning observation with four type sensors at the International Space Station (ISS). One of the sensors is very high frequency interferometer: VITF. The objective of the VITF is to locate the radiation source of received signals with two very high frequency interferometer (VHF) sensors attached on the ISS. Lightning and sprite imager: LSI is also one of the optical sensor for the observation of lightning and sprite. The LSI consists of two CMOS sensors. The image captured with the LSI gives us an information of lighting position. While the VITF has the two sensors. Although the VITF is able to estimate the direction of arrival estimation using the radio interferometric technique, we cannot locate the radiation source position. The location method are used as two direction of arrival (DOA) estimation techniques, which are the interferometric technique and based on the measurement of the group delay of the received signals. The combination of the two techniques gives us the two possible position of the radiation source when an altitude of a radiation source is assumed. The initial comparison with the optical lightning position captured with LSI are reported.
  • Yukihiro Takahashi, Mitsuteru Sato, Kozo Yamashita
    2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) 2014 [Refereed][Not invited]
  • CubeSat mission for UV-Visible observations of meteors from space: S-CUBE (S3: Shootingstar Sensing Satellite)
    R Ishimaru, Y. Sakamoto, M. Kobayashi, S. Fujita, T. Gonai, H. Senshu, K. Wada, M, Yamada, K. Kurosawa, S. Hosokawa, K. Yoshida, M. Sato, Y. Takahashi, T. Matsui
    LPS XXXXV, Abstract 1846  2014 [Not refereed][Not invited]
  • Hiroshi Kikuchi, Tomoo Ushio, Takeshi Morimoto, Mitsuteru Sato, Atsushi Yamazaki, Makoto Suzuki
    2014 INTERNATIONAL SYMPOSIUM ON ELECTROMAGNETIC COMPATIBILITY, TOKYO (EMC'14/TOKYO) 398 - 401 2158-110X 2014 [Refereed][Not invited]
     
    Since 2012, the global lightning and sprite measurements (GLIMS) mission has been conducted on the exposed facility of Japanese experiment module (JEM-EF) of the international space station (ISS). In this mission, the VHF broadband digital interferometer (VITF) attached on JEM-EF is designed to estimate the direction of arrival of electromagnetic waves. The VITF has the bandwidth from 70 MHz to 100 MHz. The electromagnetic radiations from lightning discharges received by two antennas are digitized by the 2-channel AD converter. We introduce the outline of the mission and the VITF. The initial observational results with the VITF of the GLIMS mission are presented. The comparison of the results of arrival direction estimation of the VITF with optical observations using two methods which are an interferometry technic and the group delay characteristic of EM waves. The results agree with the position of the lightning emission captured by the LSI.
  • Tomoo Ushio, Mitsuteru Sato, Takeshi Morimoto, Hiroshi Kikuchi, Makoto Suzuki, Atsushi Yamazaki, Yasuhide Hobara, Toru Adachi
    2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) 2014 [Refereed][Not invited]
     
    The Global Lightning and sprIte MeasurementS (GLIMS) on the International Space Station (ISS) is a mission to detect and locate optical transient luminous events (TLEs) and its associated lightning simultaneously from the non-sun synchronous orbit, and is scheduled to be launch from Japan in January, 2012 as part of the multi-mission consolidated equipment on Japanese Exposure Module (JEM). Our mission goals are (1) to detect and locate lightning and sprite within storm scale resolution over a large region of the Earth's surface along the orbital track of the ISS without any bias, (2) to clarify the generation mechanism of sprite, and (3) to identify the occurrence conditions of TLEs. To achieve these goals, two CMOS cameras, six Photometers, VLF receiver, and VHF interferometer with two antennas, are installed at the bottom of the module to observe the TLEs as well as causative lighting discharges at nadir direction during day and night time. Though the luminous events so-called sprite, elves and jets have been investigated by numerous researchers all over the world based mainly on the ground observations, some important problems have not been fully understood yet such as generation mechanisms of columniform fine structure and horizontal offset of some sprites from the parent lightning discharges. In the JEM-GLIMS mission, observations from our synchronized sensors are going to shed light on above-mentioned unsolved problems regarding TLEs as well as causative lighting discharges. In this presentation, the scientific background, instrumentation, project summaries and initial observation results are given.
  • An ELF Signal Associated with a Positive GC Lightning Event in Winter
    Honma. N, Y. Hongo, D. Tsurushima, F. Tsuchiya, M. Sato, Y. Takahashi
    Proc. 23nd International Lightning Detection Conf. 2014 [Not refereed][Not invited]
  • Roy Yaniv, Yoav Yair, Colin Price, Jo'zsef Bor, Mitsutero Sato, Yasuhide Hobara, Steve Cummer, Jingbo Li, Adam Devir
    JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS 107 60 - 67 1364-6826 2014/01 [Refereed][Not invited]
     
    Optical observations of 66 sprites, using a calibrated commercial CCD camera, were conducted in 20092010 and 2010-2011 winter seasons as part of the ILAN (Imaging of Lightning And Nocturnal flashes) campaign in the vicinity of Israel and the eastern Mediterranean. We looked for correlations between the properties of parent lightning (specifically, the charge moment change; CMC) to the properties of column sprites, such as the measured radiance, the length and the number of column elements in each sprite event. The brightness of sprites positively correlates with the CMC (0.7) and so does the length of sprite elements (0.83). These results are in agreement with previous studies, and support the QE model of sprite generation. (C) 2013 Elsevier Ltd. All rights reserved.
  • Nadir Observations of Lightning and TLEs by JEM-GLIMS
    M. Sato, T. Ushio, T. Morimoto, M. Suzuki, A. Yamazaki, M. Kikuchi, Y. Takahashi, I. Umran, L. Ivan, Y. Hobara
    EGU General Assembly 2013 --  2013/04 [Refereed][Not invited]
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, M. Ambrosio, L. Anchordoqui, A. Anzalone, Y. Arai, C. Aramo, K. Asano, M. Ave, P. Barrillon, T. Batsch, J. Bayer, T. Belenguer, R. Bellotti, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, J. Biccki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J. -N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, O. Catalano, A. Cellino, M. Chikawa, M. J. Christi, V. Connaughton, J. F. Cortes, H. J. Crawford, R. Cremonini, S. Csorna, J. C. D'Olivo, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, L. del Peral, A. Dell'Oro, M. P. De Pascale, M. Di Martino, G. Distratis, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, A. Franceschi, J. Fujimoto, P. Galeotti, G. Garipov, J. Geary, U. G. Giaccari, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, T. Iguchi, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, S. H. Ko, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, E. Kuznetsov, G. La Rosa, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, L. Marcelli, A. Marini, G. Martin-Chassard, O. Martinez, G. Masciantonio, K. Mase, R. Matev, A. Maurissen, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, D. Monnier-Ragaigne, J. A. Morales de los Rios, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, J. W. Nam, S. Nam, K. Nam, T. Napolitano, D. Naumov, A. Neronov, K. Nomoto, T. Ogawa, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, N. Pacheco, M. I. Panasyuk, E. Parizot, I. H. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, T. Peter, P. Picozza, A. Pollini, H. Prieto, P. Reardon, M. Reinabi, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, M. Scuderi, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozigbio, H. H. Silva Lopez, J. Sledd, K. Slomiriska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, T. Tomida, N. Tone, F. Trillaud, R. Tsenov, K. Tsuno, T. Tymieniecka, Y. Uchihori, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, A. Zamora, A. Zuccaro Marchi
    ASTROPARTICLE PHYSICS 44 76 - 90 0927-6505 2013/04 [Refereed][Not invited]
     
    We evaluate the exposure during nadir observations with JEM-EUSO, the Extreme Universe Space Observatory, on-board the Japanese Experiment Module of the International Space Station. Designed as a mission to explore the extreme energy Universe from space, JEM-EUSO will monitor the Earth's nighttime atmosphere to record the ultraviolet light from tracks generated by extensive air showers initiated by ultra-high energy cosmic rays. In the present work, we discuss the particularities of space-based observation and we compute the annual exposure in nadir observation. The results are based on studies of the expected trigger aperture and observational duty cycle, as well as, on the investigations of the effects of clouds and different types of background light. We show that the annual exposure is about one order of magnitude higher than those of the presently operating ground-based observatories. (C) 2013 Elsevier B.V. All rights reserved.
  • Makoto Taguchi, Tetsuya Fukuhara, Masahiko Futaguchi, Mitsuteru Sato, Takeshi Imamura, Kazuaki Mitsuyama, Masato Nakamura, Munetaka Ueno, Makoto Suzuki, Naomoto Iwagami, George L. Hashimoto
    ICARUS 219 (1) 502 - 504 0019-1035 2012/05 [Refereed][Not invited]
     
    Mid-infrared images of almost the entire Venus nightside hemisphere obtained by the Longwave Infrared Camera (LIR) onboard Akatsuki on December 9 and 10, 2010 reveal that the brightness temperature of the cloud-top ranges from 237 K in the cold polar collars to 243 K in the equatorial region, significantly higher than the values obtained by Venera 15. Other characteristic features of the temperature distributions observed are zonal belt structures seen in the middle and low latitudes and patchy temperature structures or quasi-periodic streaks extending in a north-south direction in the northern middle latitudes and southern low latitudes. (c) 2012 Elsevier Inc. All rights reserved.
  • Makoto Watanabe, Yukihiro Takahashi, Mitsuteru Sato, Shigeto Watanabe, Tetsuya Fukuhara, Ko Hamamoto, Akihito Ozaki
    GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY IV 8446 84462O  0277-786X 2012 [Not refereed][Not invited]
     
    We have built a visible multi-spectral imager (MSI) for the 1.6-m Pirka telescope of the Hokkaido University in Hokkaido, Japan. The instrument is equipped with two liquid crystal tunable filters and a 512 x 512 pixel EMCCD camera. One of the major purposes of this instrument is to obtain multi-spectral images (series of narrow-band images at many different wavelengths) of the solar planets rapidly. These tunable filters are a Lyot filter with liquid crystal variable retarders and thus can tune the transmitting wavelength rapidly without moving parts. Their spectral ranges are 400-720 nm and 650-1100 nm and the bandwidth is typically 10 nm on both filters. The EMCCD camera can obtain images at a frame rate of about 32 Hz, which also enables us to improve the spatial resolution with the shift-and-add or the Lucky imaging techniques. The field of view is 3.3 x 3.3 arcmin with a pixel scale of 0.39 arcsec pixel(-1). The instrument also has UBV RI-band broad-band filters and several narrow-band filters. MSI is mounted at the f/12 Cassegrain focus of the telescope. It had the first light on February 2011, and then have been used for several astronomical and planetary science programs as a major facility instrument at this telescope. We describe the design, construction, integration, and performance of this multi-spectral imager.
  • Yaegashi, A, T. Sakanoi, R. Kataoka, K. Asamura, Y. Miyoshi, M. Sato, S. Okano
    J. Geophys. Res. 116 (5) A00K04  2169-9402 2011/05/10 [Refereed][Not invited]
  • Ayumi Yaegashi, Takeshi Sakanoi, Ryuho Kataoka, Kazushi Asamura, Yoshizumi Miyoshi, Mitsuteru Sato, Shoichi Okano
    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 116 A00K04  0148-0227 2011/05 [Refereed][Not invited]
     
    We conducted high-speed imaging observations of flickering aurora at 100 Hz sampling rate using electron multiplying charge-coupled device in Alaska during 2009-2010 winter season. We detected various types of flickering aurora, including drifting and rotating features at a frequency below 15 Hz. We identified, for the first time, flickering stripes and some other unusual flickering events at frequency of higher than 20 Hz on the imaging observations. A dispersion relation derived from a statistical analysis of observed images is compared with the theoretical dispersion curve of O(+) electromagnetic ion cyclotron (EMIC) waves. The frequencies and spatial scales calculated from a coherence/phase analysis based on an interference theory are consistent with the wave dispersion relation derived from the statistical analysis, suggesting that the obtained results are essentially consistent with the scenario that the interference of EMIC waves produces the observed dispersion relation of flickering aurora. Furthermore, flickering frequencies higher than 20 Hz are confirmed from our observations, which are higher than expected frequency of O(+) EMIC waves at altitudes of several thousand kilometers. We therefore suggest that high-frequency waves such as He(+) and H(+) EMIC waves may also contribute to produce a significant fraction of flickering aurora.
  • Y. T. Tanaka, M. Hayakawa, Y. Hobara, A. P. Nickolaenko, K. Yamashita, M. Sato, Y. Takahashi, T. Terasawa, T. Takahashi
    GEOPHYSICAL RESEARCH LETTERS 38 L08805  0094-8276 2011/04 [Refereed][Not invited]
     
    We report on the first clear detection of transient Extremely-Low-Frequency (ELF) signal caused by an extremely intense cosmic gamma-ray flare. On 2004 December 27, the brightest gamma-ray flare ever recorded was observed by numerous satellites. A transient ELF emission observed at Moshiri and Onagawa in Japan exactly coincided with the peak time of the flare, and its wide pulse width of similar to 40 ms disfavors the possibility of lightning origin. Furthermore, the two horizontal components of ELF magnetic field data recorded at Esrange in Sweden showed clear transient Schumann resonance waveforms. The source direction determined by the Lissajous method roughly corresponds to the subflare point. The chance probability that a sprite occurs within 30 ms of the peak flare time is similar to 0.025%, which again clearly excludes the sprite origin. Thus, a bright cosmic gamma-ray flare is a new source of transient ELF radio signals observed on the Earth, although the emission mechanism needs to be clarified in future. Citation: Tanaka, Y. T., M. Hayakawa, Y. Hobara, A. P. Nickolaenko, K. Yamashita, M. Sato, Y. Takahashi, T. Terasawa, and T. Takahashi (2011), Detection of transient ELF emission caused by the extremely intense cosmic gamma-ray flare of 27 December 2004, Geophys. Res. Lett., 38, L08805, doi: 10.1029/2011GL047008.
  • Peng K. Hong, Hiroko Miyahara, Yusuke Yokoyama, Yukihiro Takahashi, Mitsuteru Sato
    JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS 73 (5-6) 587 - 591 1364-6826 2011/04 [Refereed][Not invited]
     
    We examined the effect of the 11-year solar cycle and quasi-biennial oscillation (QBO) on the similar to 27-day solar rotational period detected in tropical convective cloud activity. We analyzed the data of outgoing longwave radiation (OLR) for AD1979-2004, dividing into four different cases by the combination of high and low solar activities in terms of the 11-year variation, and easterly and westerly stratospheric winds associated with QBO. As a result, similar to 27-day variation has been most significantly detected in high solar activity period around the Indo-Pacific Warm Pool. Based on correlation analysis, we find that solar rotation signal can explain 10-20% of OLR variability around the tropical warm pool region during the high solar activity period. The spatial distribution has been, however, apparently different according to the phases of QBO. It is suggested that the 11-year solar cycle and stratospheric QBO have a possibility to cause large-scale oceanic dipole phenomena. (C) 2010 Elsevier Ltd. All rights reserved.
  • Kozo Yamashita, Yukihiro Takahashi, Mitsuteru Sato, Hiromi Kase
    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 116 A00E61  2169-9380 2011/02 [Refereed][Not invited]
     
    The global observation of cloud-to-ground (CG) discharges based on ELF measurements provides essential information, including vertical charge moment (Qdl) for investigations of global-scale thunderstorm activity. However, the geolocating method by direction finding of sferics in the frequency range of 1-100 Hz has a rather large error, on the order of 1000 km, even for the CGs with relatively large Qdl (>1000 C-km). Here we improve the methods for geolocation and estimation of Qdl, which are applicable to smaller CGs with Qdl down to 470 C-km, making use of the time-of-arrival method and the high correlation between Qdl and the peak amplitude of ELF sferics. The evaluated average error in geolocation, comparing with World Wide Lightning Location Network data, is 680 km. By this improved method, CGs with Qdl of <470 C-km can be detected at any location in the world. In the preliminary analysis for the year of 2004, the number of CGs whose location and Qdl are determined is about a million events per month, roughly 10-30 times compared to previous studies by ELF measurement, enabling an investigation of the day-to-day variations of the global CG distribution with transferred charge amount. The combination of accurate geolocation and the uniformity of detection show active regions in the three main areas: Africa, South America, and the Maritime Continent. In addition, minor thunderstorm areas in Japan, the Mediterranean Sea, and the Pacific Ocean can be monitored.
  • Kozo Yamashita, Yukihiro Takahashi, Mitsuteru Sato, Hiromi Kase
    Journal of Geophysical Research: Space Physics 116 (2) 2169-9402 2011 [Refereed][Not invited]
     
    The global observation of cloud-to-ground (CG) discharges based on ELF measurements provides essential information, including vertical charge moment (Qdl) for investigations of global-scale thunderstorm activity. However, the geolocating method by direction finding of sferics in the frequency range of 1-100 Hz has a rather large error, on the order of 1000 km, even for the CGs with relatively large Qdl (> 1000 C-km). Here we improve the methods for geolocation and estimation of Qdl, which are applicable to smaller CGs with Qdl down to 470 C-km, making use of the time-of-arrival method and the high correlation between Qdl and the peak amplitude of ELF sferics. The evaluated average error in geolocation, comparing with World Wide Lightning Location Network data, is 680 km. By this improved method, CGs with Qdl of < 470 C-km can be detected at any location in the world. In the preliminary analysis for the year of 2004, the number of CGs whose location and Qdl are determined is about a million events per month, roughly 10-30 times compared to previous studies by ELF measurement, enabling an investigation of the day-to-day variations of the global CG distribution with transferred charge amount. The combination of accurate geolocation and the uniformity of detection show active regions in the three main areas: Africa, South America, and the Maritime Continent. In addition, minor thunderstorm areas in Japan, the Mediterranean Sea, and the Pacific Ocean can be monitored. Copyright 2011 by the American Geophysical Union.
  • Tetsuya Fukuhara, Makoto Taguchi, Takeshi Imamura, Masato Nakamura, Munetaka Ueno, Makoto Suzuki, Naomoto Iwagami, Mitsuteru Sato, Kazuaki Mitsuyama, George L. Hashimoto, Ryo Ohshima, Toru Kouyama, Hiroki Ando, Masahiko Futaguchi
    EARTH PLANETS AND SPACE 63 (9) 1009 - 1018 1880-5981 2011 [Refereed][Not invited]
     
    The Longwave Infrared Camera (LIR) is one of a suite of cameras onboard the Venus orbiter Akatsuki. It will take images of thermal radiation in the wavelength range of 8-12 mu m emitted by the Venus cloud tops. The use of an uncooled micro-bolometer array as an infrared image sensor makes LIR a lightweight, small and low-power consumption instrument with a required noise equivalent temperature difference of 0.3 K. Temperature and horizontal wind fields at the cloud-top will be retrieved for both dayside and nightside with equal quality. This will provide key observations to understand the mechanism of super rotation and the thermal budget of the planet. LIR will also monitor variations of the polar dipole and collar which are characteristic thermal features in the Venusian atmosphere. Mechanisms of the upper-cloud formation will be investigated using sequences of close-up images. The morphology of the nightside upper cloud will be studied in detail for the first time.
  • Tomoo Ushio, Mitsuteru Sato, Takeshi Morimoto, Makoto Suzuki, Hiroshi Kikuchi, Atsushi Yamazaki, Yukihiro Takahashi, Yasuhide Hobara, Umran Inan, Ivan Linscott, Yuji Sakamoto, Ryohei Ishida, Masayuki Kikuchi, Kazuya Yoshida, Zen Ichiro Kawasaki
    IEEJ Transactions on Fundamentals and Materials 131 (12) 971 - 976 0385-4205 2011 [Refereed][Not invited]
     
    Global Lightning and sprIte MeasurementS (GLIMS) is a mission on the International Space Station (ISS) to detect and locate optical transient luminous events (TLEs) and associated lightning simultaneously from the non-sun-synchronous orbit. It is scheduled to be launched from Japan in January, 2012 as part of the multi-mission consolidated equipment on the Japanese Exposure Module (JEM). Our mission's goals are (1) to detect and locate lightning and sprites within storm scale resolution over a large region of the Earth's surface along the orbital track of the ISS without any bias, (2) to clarify the mechanism by which sprites are generated, and (3) to identify the conditions under which TLEs occur. To achieve these goals, two CMOS cameras, six Photometers, a VLF receiver and VHF interferometer with two antennas are installed at the bottom of the module to observe the TLEs, as well as causative lightning discharges at nadir direction during day and night time. Though the luminous events' so-called sprites, elves and jets have been investigated by numerous researchers all over the world based mainly on ground observations, some important problems have not been fully understood yet. These include the generation mechanisms of columniform fine structures and horizontal offset of some sprites from the parent lightning discharges. In the JEM-GLIMS mission, observations from our synchronized sensors will shed light on the unsolved problems mentioned above regarding TLEs and causative lightning discharges. In this presentation scientific background, instrumentation, and project summaries are given. © 2011 The Institute of Electrical Engineers of Japan.
  • Takeshi Morimoto, Hiroshi Kikuchi, Mitsuteru Sato, Makoto Suzuki, Atsushi Yamazaki, Tomoo Ushio
    IEEJ Transactions on Fundamentals and Materials 131 (12) 977 - 982 0385-4205 2011 [Refereed][Not invited]
     
    Global Lightning and sprIte MeaSurements (GLIMS) mission is scheduled on Exposed Facility of Japanese Experiment Module (JEM-EF) of the International Space Station (ISS). This paper introduced an electromagnetic (EM) payload of JEM-GLIMS mission, very high frequency (VHF) broadband digital In TerFerometer (VITF). VITF consists of a pair of VHF broadband antennas and electronics to record EM waveforms from lightning discharges. It is designed to estimate the direction-of-arrival with about 10 km resolution that is equivalent to the scale of a thundercloud. It means that VITF is able to monitor thunderclouds with lightning activities globally. Comprehensive observations with the optical payloads of JEM-GLIMS mission for lightning activities and related transient luminous events (TLEs) are expected to give us many scientific impacts to the field. The developments of VITF are based on the heritage of VHF sensor on Maido-1 satellite. © 2011 The Institute of Electrical Engineers of Japan.
  • Masayuki Kikuchi, Mitsuteru Sato, Atsushi Yamazaki, Makoto Suzuki, Tomoo Ushio
    IEEJ Transactions on Fundamentals and Materials 131 (12) 989 - 993 0385-4205 2011 [Refereed][Not invited]
     
    A project to observe lightning and sprites from the International Space Station (ISS), with altitude of 407 km and inclination of 51.6°, is planned for 2012. GLIMS (global lightning and sprite measurements) is an instrument designed for this project, and it includes a CMOS camera, photomultipliers, a VLF receiver, and a VHF interferometer. This is the first project for simultaneous measurements of lightning, sprites, and radiowaves from lightning simultaneously. The sensors used for GLIMS were developed based on previous satellite projects. However, for this project, the sensors used needed to be synchronized, and controlled through the Japanese experiment module (JEM) interface. A science data-handling unit (SHU) was newly developed for this purpose; it included a function for suppressing data traffic using a high-speed lossless compression code (HIREW). © 2011 The Institute of Electrical Engineers of Japan.
  • Mitsuteru Sato, Yukihiro Takahashi, Makoto Suzuki, Atsushi Yamazaki, Tomoo Ushio
    IEEJ Transactions on Fundamentals and Materials 131 (12) 1000 - 1005 0385-4205 2011 [Refereed][Not invited]
     
    Six-channel spectrophotometers (PH) are the science instruments of JEM-GLIMS to measure absolute intensity of the emission originated from lightning discharges and upper atmospheric transient luminous events (TLEs). PH unit-1 (PH-U1) consists of four spectrophotometer channels named from PH1 to PH4, while PH unit-2 (PH-U2) two spectrophotometer channels named PH5 and PH6. Optical filters of these spectrophotometers are selected to detect TLE emission lines of N 2 1PG, N 2 2PG, N +2 1NG, and N 2 LBH. Since the bandwidth of the optical filter of PH2,3,5, and 6 is 10 nm and since PH1 measures NUV emission, photomultiplier tubes with high-voltage converters are used as a photon detector. To the contrary, PH4 uses a photodiode as a photon detector because the pass-band of the optical filter is enough wide to detect transient optical emission. Though PH does not equip spatial resolution, it can acquire light curve data with a high time resolution of 50 μs with a 12-bit resolution. Thus, the combinational analysis of PH data and Lightning and Sprite Imager (LSI) data, it is possible to clarify the relationship between TLEs and their parent lightning discharges, the occurrence condition of TLEs, and the energy of the electrons which excite TLE emission. © 2011 The Institute of Electrical Engineers of Japan.
  • Mitsuteru Sato, Yukihiro Takahashi, Masayuki Kikuchi, Makoto Suzuki, Atsushi Yamazaki, Tomoo Ushio
    IEEJ Transactions on Fundamentals and Materials 131 (12) 994 - 999 0385-4205 2011 [Refereed][Not invited]
     
    Lightning and Sprite Imager (LSI) is a science instrument of JEM-GLIMS to capture images of lightning discharges and upper atmospheric transient luminous events (TLEs), such as sprites, elves and blue jets. LSI consists of two CMOS cameras; one is a wide-band camera named LSI-1 that is equipped with an optical filter whose pass-band ranges from 765nm to 830nm, the other is a narrow-band camera named LSI-2 that is equipped with an optical filter whose transmittance centers at the wavelength of 762 nm and has band width of 14 nm. From the comparison of LSI-1 images with LSI-2 images the time evolution and spatial distribution of lightning discharges and TLEs can be identified. Since the telemetry speed provided for JEM-GLIMS is limited, LSI images will be acquired not continuously but intermittently according to the onboard event trigger logic. This trigger logic selects only the transient optical flashes caused by lightning discharges or TLEs effectively. © 2011 The Institute of Electrical Engineers of Japan.
  • Y. Takahashi, A. Yoshida, M. Sato, T. Adachi, S. Kondo, R. -R. Hsu, H. -T. Su, A. B. Chen, S. B. Mende, H. U. Frey, L. -C. Lee
    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 115 A00E55  0148-0227 2010/09 [Refereed][Not invited]
     
    Although the Quasi-electrostatic (QE) model has been considered a basic mechanism for describing sprite generation, the relationship between sprite luminosity and the charge moment change (CMC) value, caused by the sprites' parent lightning has not been examined quantitatively. CMC value represents the energy of cloud-to-ground discharge (CG) and the electric field intensity above the thunderstorm. We focused on the data obtained in 2004, in which both ISUAL on board the FORMOSAT-2 satellite and the Tohoku ELF network were operated throughout one year. We could estimate the absolute luminous intensity of sprites free from atmospheric influence with the ISUAL/Array Photometer (AP) and investigated its relationship to the charge moment of parent lightning. Absolute optical energies emitted from sprites were estimated for 14 streamer-type sprites for the first time. The averages of the time-integrated optical energies are 176 kJ and 119 kJ for the N2 1PG and N2 2PG bands, respectively. Furthermore, the optical energies and the charge moments of their parent lightning estimated with ELF data show a high correlation (correlation coefficient = 0.93), that is consistent, qualitatively, with the QE model. This relationship predicts that the 50% occurrence probability is located at similar to 600 C km, which coincides with previous statistical studies.
  • Y. Takahashi, A. Yoshida, M. Sato, T. Adachi, S. Kondo, R. R. Hsu, H. T. Su, A. B. Chen, S. B. Mende, H. U. Frey, L. C. Lee
    Journal of Geophysical Research: Space Physics 115 (9) 2169-9402 2010 [Refereed][Not invited]
     
    Although the Quasi-electrostatic (QE) model has been considered a basic mechanism for describing sprite generation, the relationship between sprite luminosity and the charge moment change (CMC) value, caused by the sprites' parent lightning has not been examined quantitatively. CMC value represents the energy of cloud-to-ground discharge (CG) and the electric field intensity above the thunderstorm. We focused on the data obtained in 2004, in which both ISUAL on board the FORMOSAT-2 satellite and the Tohoku ELF network were operated throughout one year. We could estimate the absolute luminous intensity of sprites free from atmospheric influence with the ISUAL/Array Photometer (AP) and investigated its relationship to the charge moment of parent lightning. Absolute optical energies emitted from sprites were estimated for 14 streamer-type sprites for the first time. The averages of the time-integrated optical energies are 176 kJ and 119 kJ for the N2 1PG and N2 2PG bands, respectively. Furthermore, the optical energies and the charge moments of their parent lightning estimated with ELF data show a high correlation (correlation coefficient = 0.93), that is consistent, qualitatively, with the QE model. This relationship predicts that the 50% occurrence probability is located at ∼600 C km, which coincides with previous statistical studies. Copyright 2010 by the American Geophysical Union.
  • SPRITE-SAT: a micro satellite for scientific observation of transient luminous events and terrestrial gamma-ray flashes
    Yoshida, K, Y. Takahashi, Y. Sakamoto, E. Ujiie, K. Takiuchi, Y. Nakazato, T. Sawakami, T. Sakanoi, Y. Kasaba, S. Kondo, K. Yamashita, S. Ueda, T. Takashima, K. Nakazawa, T. Mitani, T. Enoto, M. Sato, U. Inan, I. Linscott, F. Bruhn, Y. Masumoto
    Trans. Soc. Aerospace Tech. Japan 8 (Tm) 7 - 12 2010 [Refereed][Not invited]
  • E. R. Williams, W. A. Lyons, Y. Hobara, V. C. Mushtak, N. Asencio, R. Boldi, J. Bor, S. A. Cummer, E. Greenberg, M. Hayakawa, R. H. Holzworth, V. Kotroni, J. Li, C. Morales, T. E. Nelson, C. Price, B. Russell, M. Sato, G. Satori, K. Shirahata, Y. Takahashi, K. Yamashita
    QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY 136 257 - 271 0035-9009 2010/01 [Refereed][Not invited]
     
    Sprites have been detected in video camera observations from Niger over mesoscale convective systems in Nigeria during the 2006 AMMA (African Monsoon Multidisciplinary Analysis) campaign The parent lightning flashes have been detected by multiple Extremely Low Frequency (ELF) receiving stations worldwide The recorded charge moments of the patent lightning flashes are often in excellent agreement between different receiving sites, and are furthermore consistent with conventional dielectric breakdown in the mesosphere as the origin of the sprites Analysis of the polarization of the horizontal magnetic field at the distant receivers provides evidence that the departure from linear magnetic polarization at ELF is caused primarily by the clay night asymmetry of the Earth-ionosphere cavity Copyright (C) 2009 Royal Meteorological Society
  • Y. Takahashi, Y. Okazaki, M. Sato, H. Miyahara, K. Sakanoi, P. K. Hong, N. Hoshino
    ATMOSPHERIC CHEMISTRY AND PHYSICS 10 (4) 1577 - 1584 1680-7316 2010 [Refereed][Not invited]
     
    Although linkages between solar activity and the earth's climate have been suggested and the 11-year cycle in solar activity evident in sunspot numbers is the most examined example of periodicity in previous studies, no quantitative evidence indicating a relationship for tropospheric phenomena has been found for a short period. Based on FFT analysis for OLR (Outgoing Longwave Radiation) compared with the F10.7 index, we clearly demonstrate a 27-day variation in the cloud amount in the region of the Western Pacific warm pool, which is only seen in the maximum years of 11-year solar activity. The average spectrum in such years also shows an enhancement in the range of the MJO (Madden-Julian Oscillation) period. Although there exist some explanations for possible mechanisms, the exact cause is unknown. Therefore, the proposed connection between 27-day cloud variation and solar cycle in the WPWP region is still a hypothesis and various kinds of varification based on other meteorological and solar parameters are strongly required.
  • れいめい衛星搭載カメラによる大気光・スプライト観測
    坂野井健, 山崎敦, 藤原均, 平原聖文, 浅村和史, 江尻省, 鈴木臣, 中村卓司, 佐藤光輝, 高橋幸弘, 岡野章一
    平成20年度宇宙科学シンポジウム集録 2009 [Not refereed][Not invited]
     
    筆頭
  • M. Sato, Y. Takahashi, A. Yoshida, T. Adachi
    JOURNAL OF PHYSICS D-APPLIED PHYSICS 41 (23) 234011  0022-3727 2008/12 [Refereed][Not invited]
     
    In order to study the temporal and regional variation of lightning occurrences and their relation to sprite activity and climate variability, we have analysed the 1-100 Hz ELF magnetic field waveform data obtained at the Syowa station in Antarctica, Onagawa in Japan and Esrange in Sweden for a one year period from September 2003 to August 2004. We have selected totally 1.7 x 105 events of transient Schumann resonances from the ELF magnetic field data whose amplitude exceeds 40 pT at all stations. Then, the lightning locations are estimated by a triangulation method with an estimation error of 0.5 Mm. It is found that in the summer season (from June to August) the lightning occurrence rates are higher in the northern hemisphere than in the southern hemisphere with large enhancements in North America, South-East Asia and the northern part of Africa. On the other hand, in the winter season ( from December to February) these rates are higher in the southern hemisphere with large enhancements in South America, Australia and the southern part of Africa. These features are consistent with the results of global lightning measurements from space conducted by the Optical Transient Detector and the Tropical Rainfall Measuring Mission satellite. Then, we have also calculated the charge moment value (Q . dl) of lightning discharges using ELF magnetic field waveform data and have estimated the distribution function of charge moments for positive cloud-to-ground (+CG) discharges and for negative cloud-to-ground (-CG) discharges. It is found that the shape of the distribution function for both +CG and -CG discharges is almost the same for all seasons and that the distribution function of -CG discharges has a steeper slope at high Q . dl than that of +CG discharges.
  • Development of the sprite and lightning imaging system onboard the SPRITE-SAT
    Sato, M, Y. Takahashi, T. Sakanoi, S. Ueda, S. Kondo, K. Yoshida, Y. Sakamoto, T. Takashima
    EOS Trans, AGU 88 (52) 2008 [Not refereed][Not invited]
  • T. Ebisuzaki, Y. Uehara, H. Ohmori, K. Kawai, Y. Kawasaki, M. Sato, Y. Takizawa, M. E. Bertaina, F. Kajino, T. Sawabe, K. Inoue, A. Sasaki, M. Sakata, Y. Yamamoto, M. Nagano, N. Inoue, T. Shibata, N. Sakaki, Y. Uchihori, Y. Takahashi, H. Shimizu, Y. Arai, Y. Kurihara, H. Fujimoto, S. Yoshida, Y. Mizumoto, S. Inoue, K. Asano, T. Sugiyama, J. Watanabe, H. Ikeda, M. Suzuki, T. Imamura, H. Yano, T. Murakami, D. Yonetoku, Y. Itow, M. Taguchi, M. Nagata, S. Nagataki, S. Abe, T. Tajima, J. H. Adams, S. Mitchell, M. J. Christl, J. Watts, A. English, Y. Takahashi, K. Pitalo, J. Hadaway, J. Geary, P. Readon, H. Crawford, C. Pennypacker, K. Arisaka, D. Cline, P. Gorodetsky, P. Salin, T. Patzark, A. Maurissen, M. Valentin
    NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS 175 (SUPPL.: COMPLETE) 237 - 240 0920-5632 2008/01 [Refereed][Not invited]
     
    The motivations, characteristics and potential performance of the JEM-EUSO project are briefly discussed.
  • Tetsuya Fukuhara, Makoto Taguchi, Takeshi Imamura, Masato Nakamura, Naomoto Iwagami, Munetaka Ueno, Makoto Suzuki, George L. Hashimotod, Mitsuteru Sato, Atsushi Yamazaki, Ryoichi Kashikawa, Isamu Higashino, Kazuhide Noguchi
    INFRARED TECHNOLOGY AND APPLICATIONS XXXIV, PTS 1 AND 2 6940 694030  0277-786X 2008 [Refereed][Not invited]
     
    The Longwave Infrared Camera (LIR), which mounts an uncooled micro-bolometer array (UMBA), is under development for the Japanese Venus orbiter mission, PLANET-C. LIR detects thermal emission from the top of the sulfur dioxide cloud in a wavelength region 8-12 mu m to map the cloud-top temperature which is typically as low as 230 K. The requirement for the noise equivalent temperature difference (NETD) is 0.3 K. Images of blackbody targets in room temperature (similar to 300 K) and low temperature (similar to 230 K) have been acquired in a vacuum environment using a prototype model of LIR, showing that the NETD of 0.2 K and 0.8 K are achieved in similar to 300 K and -230 K, respectively. We expect that the requirement of NETD < 0.3 K for similar to 230 K targets will be achieved by averaging several tens of images which are acquired within a few minutes. The vibration test for the UMBA was also carried out and the result showed the UMBA survived without any pixel defects or malfunctions. The tolerance to high-energy protons was tested and verified using a commercial camera in which a same type of UMBA is mounted. Based on these results, a flight model is now being manufactured with minor modifications from the prototype.
  • Atmospheric monitoring system of JEM-EUSO mission
    Mitev, V, M. Sato, T. Ebisuzaki, Y. Takizawa, Y. Kawasaki, R. Matthey, JEM-EUSO Collaboration
    International Journal of Modern Physics A 5 1053 - 1056 2007 [Refereed][Not invited]
  • Y. Kawasaki, M. E. Bertaina, N. Sakaki, H. M. Shimizu, N. Inoue, S. Hasegawa, I. Ohtsu, T. Adachi, T. Ebisuzaki, K. Hirota, K. Ikeda, F. Kajino, T. Morishima, M. Nagano, M. Sato, T. Sawabe, T. Shibata, T. Shinohara, M. Takeda, Y. Takizawa, Y. Uchihori, Y. Wada
    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT 564 (1) 378 - 394 0168-9002 2006/08 [Refereed][Not invited]
     
    We have developed and tested a new type of multi-anode photomultiplier: Hamamatsu R8900-03 series. The main feature of the R8900-03 series is a highly sensitive surface: similar to 83% of the physical area. In this paper we report on the results of measurements we performed to check several parameters of this new type of photomultiplier. R8900-03 photomultipliers are devices suitable for experiments where large collection area and uniform detection efficiency are essential characteristics. (c) 2006 Elsevier B.V. All rights reserved.
  • Y Kawasaki, M Bertaina, T Ebisuzaki, F Kajino, Y Miyazaki, M Nagano, N Sakaki, M Sato, HM Shimizu, Y Takizawa, M Ameri, O Catalano, S Cuneo, F Fontanelli, Gracco, V, P Musico, M Pallavicini, A Petrolini, R Pratolongo, M Sannino, N Bleurvacq, F Cadoux, C Chapron, P Gorodetzky, P Nedelec, T Patzak, E Plagnol, Y Takahashi
    INTERNATIONAL JOURNAL OF MODERN PHYSICS A 20 (29) 6890 - 6893 0217-751X 2005/11 [Refereed][Not invited]
     
    The Extreme Universe Space Observatory (EUSO) is a space mission to study extremely high-energy cosmic rays. The EUSO instrument is a wide-angle refractive telescope in near-ultraviolet wavelength region to observe time-resolved atmospheric fluorescence images of the extensive air showers from the International Space Station. The Focal surface is an aspherical curved surface, and its area amounts to about 4.5 m(2). The focal surface detector is designed as a mosaic of multianode photomultipliers (MAPMT) for the single photoelectron counting capability. The strongest requirement for the focal surface detector is the maximization of the photon detection efficiency together with the uniformity over the focal surface. We have developed a new type of MAPMT. It is modified from the ordinary one and has a grid between the photocathode and the first dynode to electrostatically demagnify the photoelectron image on the dynode. We are also developing the HV supply system for a great number of MAPMTs. EUSO experiments the day-time and night-time every 90 minutes. The heat flow must be considered to stabilize the PMT characteristics, in parallel with the heat dissipation of the electronics attached on the focal surface supporting structure.
  • M Bertaina, T Ebisuzaki, K Hirota, Y Kawasaki, N Sakaki, M Sato, HM Shimizu, T Shinohara, Y Takizawa
    INTERNATIONAL JOURNAL OF MODERN PHYSICS A 20 (29) 6872 - 6874 0217-751X 2005/11 [Refereed][Not invited]
     
    RIKEN has developed in collaboration with Hamamatsu a new type of Multi Anode Photomultiplier (MAPMT), R8900 series, with a large sensitive area of similar to 83% of the physical surface. The performance of R8900 is reviewed in the following. RIKEN has also manufactured a new type of wavelength shifter (w.s.) film to shift near-UV light (330 divided by 400 nm) to visible one. This film uses POPOP as a shifter and EPO-TEX as a substrate. The quantum efficiency of the film reaches similar to 80%.
  • M Sato, T Ebisuzaki, Y Takizawa, Y Kawasaki, N Sakaki, M Bertaina, HM Shimizu, Y Takahashi, T Adachi
    INTERNATIONAL JOURNAL OF MODERN PHYSICS A 20 (29) 6903 - 6905 0217-751X 2005/11 [Refereed][Not invited]
     
    In this study we present possibility of continuous measurements of lightning-associated transient luminous events (sprites, elves and blue jets) from the ISS altitude using the EUSO telescope. From global lightning data we estimated possible detection rates of lightning and TLEs. We also estimated photon numbers and optical spectra of TLEs in the near-ultraviolet region (300 - 400 nm) where the fluorescence emission caused by CRs exists. These results imply that EUSO has enough capabilities to monitor not only super-GZK CRs but also global lightning and TLEs.
  • Mitsuteru Sato, Hiroshi Fukunishi
    Geophysical Research Letters 32 (12) 1 - 4 0094-8276 2005/06/28 [Refereed][Not invited]
     
    We report new evidence for a link between lightning activity and tropical upper cloud coverage. Using 1 - 100 Hz ELF magnetic field waveform data obtained at Syowa station, we analyzed Schumann resonance (SR) spectral intensity variation to investigate characteristics of lightning activity changes. Further, we performed the cross-spectral analysis between the spectral intensity variation and the tropical upper cloud coverage at high altitude derived from infrared cloud images. It is found that the tropical upper cloud coverage and the lightning activity change with the same periodicity and a clear anti-phase relation. These results imply that the lightning activity is closely related to the meteorological dynamics in the troposphere. This fact demonstrates that tropical upper cloud coverage may be continuously monitored by SRs measured at a single site on the Earth's surface. Copyright 2005 by the American Geophysical Union.
  • T. Adachi, H. Fukunishi, Yukihiro Takahashi, M. Sato, A. Ohkubo, Katsura Yamamoto
    Journal of Geophysical Research D: Atmospheres 110 (11) 1 - 11 0148-0227 2005/06/16 [Refereed][Not invited]
     
    In this work, we analyze 67 sprite events observed during the winter sprite campaign carried out in Japan from 1998 to 2003. Our aim is to clarify the relationship between winter sprites in Japan and the characteristics of their parent thunderstorm systems. Combining optical data of sprites, various meteorological data such as cloud maps obtained from the Geostationary Meteorological Satellite-5, and precipitation maps obtained from Doppler radars as well as lightning detection network data, we classify sprite-producing thunderstorm systems into four categories: (1) those associated with the cold front over the Sea of Japan, (2) those developing in the Japan Sea Polar Air Mass Convergence Zone, (3) those developing in local low-pressure areas over the Pacific Ocean, and (4) those developing ∼200-900 km behind the cold front over the Pacific Ocean. These thunderstorm systems have average cloud top temperatures ranging from -25 to -40°C and average horizontal areas of 8500-40,500 km2 at the -20°C isotherm. They are much smaller than thunderstorm systems over the U.S. high plains in the summertime. The average maximum occurrence rate of sprites is 7.7 per hour in category 1, while the occurrence rates in categories 2-4 are only 2-3 per hour. In each of the four categories of thunderstorm systems, winter sprites in Japan tend to be induced by positive cloud-to-ground lightning discharges occurring in the convective core region during the developing stage where and when convection becomes most active spatially and temporally. Copyright 2005 by the American Geophysical Union.
  • T Adachi, H Fukunishi, Y Takahashi, M Sato, A Ohkubo, K Yamamoto
    JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES 110 (D11) D11203  2169-897X 2005/06 [Refereed][Not invited]
     
    [1] In this work, we analyze 67 sprite events observed during the winter sprite campaign carried out in Japan from 1998 to 2003. Our aim is to clarify the relationship between winter sprites in Japan and the characteristics of their parent thunderstorm systems. Combining optical data of sprites, various meteorological data such as cloud maps obtained from the Geostationary Meteorological Satellite-5, and precipitation maps obtained from Doppler radars as well as lightning detection network data, we classify sprite-producing thunderstorm systems into four categories: ( 1) those associated with the cold front over the Sea of Japan, ( 2) those developing in the Japan Sea Polar Air Mass Convergence Zone, ( 3) those developing in local low-pressure areas over the Pacific Ocean, and ( 4) those developing similar to 200 - 900 km behind the cold front over the Pacific Ocean. These thunderstorm systems have average cloud top temperatures ranging from - 25 to - 40 degrees C and average horizontal areas of 8500 - 40,500 km(2) at the - 20 degrees C isotherm. They are much smaller than thunderstorm systems over the U. S. high plains in the summertime. The average maximum occurrence rate of sprites is 7.7 per hour in category 1, while the occurrence rates in categories 2 - 4 are only 2 - 3 per hour. In each of the four categories of thunderstorm systems, winter sprites in Japan tend to be induced by positive cloud-to-ground lightning discharges occurring in the convective core region during the developing stage where and when convection becomes most active spatially and temporally.
  • M. Sato, Y. Takizawa, Y. Kawasaki, M. Bertaina, T. Ebisuzaki, Y-H. Takahashi, D. Lebrun
    Proceedings of the 29th International Cosmic Ray Conference Vol 8: HE 1.5 201 - 204 2005 [Refereed][Not invited]
     
    In this study we present possibility of continuous measurements of lightning-associated transient luminous events (TLEs) from the international space station using the Extreme Universe Space Observatory (EUSO) telescope. From global lightning data we estimated possible detection rates of lightning and TLEs. We also estimated photon numbers and optical spectra of TLEs in the near-ultraviolet region (300-400 nm) where the fluorescence emission caused by CRs exists. These results imply that EUSO has enough capabilities to monitor not only UHECRs but also global lightning and TLEs. We are developing a new-type of high-voltage divider for multi-anode photomultiplier tubes (MAPMTs) which can automatically change the gain level rapidly (< 350 mu s) and which enable us to carry out both UHECR and TLE observations. An electronic design and performances of the divider circuit will be presented.
  • Y Yair, C Price, B Ziv, PL Israelevich, DD Sentman, FT Sao-Sabbas, AD Devir, M Sato, CJ Rodger, M Moalem, E Greenberg, O Yaron
    GEOPHYSICAL RESEARCH LETTERS 32 (2) L20801  0094-8276 2005/01 [Refereed][Not invited]
     
    We report an observation of an unusual transient luminous event (TLE) detected in the near IR, south of Madagascar above the Indian Ocean. The event was imaged from the space shuttle Columbia during the MEIDEX sprite campaign [Yair et al., 2004]. It was delayed 0.23 seconds from a preceding visual lightning flash which was horizontally displaced >1000 km from the event. The calculated brightness in the 860 (+/-50) nm filter was similar to310+/- 30 kR, and the morphology of the emitting volume did not resemble any known class of TLE (i.e., sprites, ELVES or halos). This TIGER event (Transient Ionospheric Glow Emission in Red) may constitute a new class of TLE, not necessarily induced by a near-by thunderstorm. We discuss possible generation mechanisms, including the conjugate sprite hypothesis caused by lightning at the magnetic mirror point, lightning-induced electron precipitation and an extraterrestrial source, meteoric or cometary.
  • N Sato, DM Wright, CW Carlson, Y Ebihara, M Sato, T Saemundsson, SE Milan, M Lester
    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 109 (A10) A10201  0148-0227 2004/10 [Refereed][Not invited]
     
    We have carried out a direct comparison of pulsating auroras observed from the ground at Syowa Station in Antarctica and on board the FAST satellite (similar to3100 km altitude), with reference to simultaneous data obtained by a Syowa-Iceland conjugate pair of observatories. The aurora at Syowa appeared as east-west aligned bands consisting of two different types: a poleward moving oscillation and a standing oscillation, each with a period of similar to6 s. Spatial and temporal variations of the downgoing high-energy (>5 keV) electron flux obtained by FAST showed a one-to-one correspondence with the optical pulsating aurora. The occurrence regions of the two different types of pulsating aurora were separated by a narrow gap (similar to7-10 km in width at 100 km altitude) in the inverted-V structure, and the gaps were colocated with the small-scale upward field-aligned currents. The time-varying magnetic fields (upward field-aligned current) observed by FAST were almost correlated (in-phase) with the downgoing electron flux (>5 keV) modulations. Both the optical emission intensity at Syowa and the downgoing high-energy electron flux (>7 keV) on board FAST showed similar to3 Hz modulation. The similar to3 Hz fine structure constituted the main body of the similar to6 s pulsating aurora. VLF wave activities were not observed by FAST in the region of pulsating aurora. The source regions of the generation or modulation of the energetic particles are estimated to be at a higher altitude than FAST, in the region of similar to2 Re to 6 Re from the satellite. This suggests that the source region is not located in the equatorial plane of the magnetosphere but is located earthward, far from the equatorial plane. The conjugate pair observations on the ground revealed that the aurora, though pulsating in both hemispheres, was not conjugate in shape, appearing as an east-west aligned band in the Southern Hemisphere but as a torch structure (omega band) in the Northern Hemisphere. The evidence presented in this study suggests that ionosphere-magnetosphere coupling processes are important in producing the pulsating aurora.
  • C Price, E Greenberg, Y Yair, G Satori, J Bor, H Fukunishi, M Sato, P Israelevich, M Moalem, A Devir, Z Levin, JH Joseph, Mayo, I, B Ziv, A Sternlieb
    GEOPHYSICAL RESEARCH LETTERS 31 (20) L20107  0094-8276 2004/10 [Refereed][Not invited]
     
    In January 2003 Transient Luminous Events (TLEs) also known as sprites and ELVES were observed by the astronauts on board of the Columbia space shuttle, during the Mediterranean Israeli Dust Experiment (MEIDEX). Throughout the 16-day mission, electromagnetic data at four ground-based Extremely Low Frequency ( ELF) stations ( Israel, Hungary, Japan and Antarctica) were collected to geo-locate and determine the parameters of the parent lightning that triggered the TLEs. From our analysis 7 ELVES and 7 sprites have been detected so far in our data. ELF transients were detected for 5 of 7 ELVES at all ground stations with accurate geo-location of these events. However, none of the sprites were associated with ELF transients. This is contrary to the present theories of TLE formation, and may require some new thinking into the mechanisms that produce sprites and ELVES.
  • T Adachi, H Fukunishi, Y Takahashi, M Sato
    GEOPHYSICAL RESEARCH LETTERS 31 (4) L04107  0094-8276 2004/02 [Refereed][Not invited]
     
    In order to elucidate the electrodynamic coupling process between sprites and their causative cloud-to-ground lightning discharges, we investigated 38 columniform sprite events observed in the wintertime sprite campaigns in Japan. By analyzing the data of sprite images, transient Schumann resonance waveforms and the JLDN/LPATS lightning detection network systems, we found that the number of columns in each sprite event was proportional to the peak current intensity of positive cloud-to-ground lightning discharges (+ CGs) while the average vertical length of columns was proportional to the charge moment of the causative + CGs. Based on these results, we suggest that electromagnetic pulses (EMPs) radiated from + CGs contribute to the formation of seeds for sprite streamers while the QE field contribute to the development of the streamers from the seeds.
  • N. Sato, D. M. Wright, C. W. Carlson, Y. Ebihara, M. Sato, T. Saemundsson, S. E. Milan, M. Lester
    Journal of Geophysical Research: Space Physics 109 (10) 2169-9402 2004 [Refereed][Not invited]
     
    We have carried out a direct comparison of pulsating auroras observed from the ground at Syowa Station in Antarctica and on board the FAST satellite (∼3100 km altitude), with reference to simultaneous data obtained by a Syowa-Iceland conjugate pair of observatories. The aurora at Syowa appeared as east-west aligned bands consisting of two different types: a poleward moving oscillation and a standing oscillation, each with a period of ∼6 s. Spatial and temporal variations of the downgoing high-energy (> 5 keV) electron flux obtained by FAST showed a one-to-one correspondence with the optical pulsating aurora. The occurrence regions of the two different types of pulsating aurora were separated by a narrow gap (∼7-10 km in width at 100 km altitude) in the inverted-V structure, and the gaps were colocated with the small-scale upward field-aligned currents. The time-varying magnetic fields (upward field-aligned current) observed by FAST were almost correlated (in-phase) with the downgoing electron flux (> 5 keV) modulations. Both the optical emission intensity at Syowa and the downgoing high-energy electron flux (> 7 keV) on board FAST showed ∼3 Hz modulation. The ∼3 Hz fine structure constituted the main body of the ∼6 s pulsating aurora. VLF wave activities were not observed by FAST in the region of pulsating aurora. The source regions of the generation or modulation of the energetic particles are estimated to be at a higher altitude than FAST, in the region of ∼2 Re to 6 Re from the satellite. This suggests that the source region is not located in the equatorial plane of the magnetosphere but is located earthward, far from the equatorial plane. The conjugate pair observations on the ground revealed that the aurora, though pulsating in both hemispheres, was not conjugate in shape, appearing as an east-west aligned band in the Southern Hemisphere but as a torch structure (omega band) in the Northern Hemisphere. The evidence presented in this study suggests that ionosphere-magnetosphere coupling processes are important in producing the pulsating aurora. Copyright 2004 by the American Geophysical Union.
  • M Sato, H Fukunishi
    GEOPHYSICAL RESEARCH LETTERS 30 (16) 1859  0094-8276 2003/08 [Refereed][Not invited]
     
    [1] We estimated locations and rates of sprite occurrences on a global scale using 1 - 100 Hz ELF magnetic field waveform data obtained at Syowa station in Antarctica and Onagawa observatory in Japan. From the ELF data obtained in a period between June 19, 2001 and January 20, 2002, we identified 715,500 events of transient Schumann resonances (SRs). The locations and polarizations of these parent cloud-to-ground (CG) discharges were determined by a triangulation method. The charge moments of these CG discharges were calculated with a normal mode expansion model of SR waves. From these results and the empirical sprite initiation probability reported by Hu et al. [ 2002], the global occurrence rate of sprites is estimated to be about 720 events/day on average. It is also found that the active regions of sprite occurrences are located in North and South America, Africa and South-East Asia.
  • HT Su, RR Hsu, AB Chen, YC Wang, WS Hsiao, WC Lai, LC Lee, M Sato, H Fukunishi
    NATURE 423 (6943) 974 - 976 0028-0836 2003/06 [Refereed][Not invited]
     
    Transient luminous events in the atmosphere, such as lighting-induced sprites(1-8) and upwardly discharging blue jets(9-14), were discovered recently in the region between thunderclouds and the ionosphere. In the conventional picture, the main components of Earth's global electric circuit(15,16) include thunderstorms, the conducting ionosphere, the downward fair-weather currents and the conducting Earth. Thunderstorms serve as one of the generators that drive current upward from cloud tops to the ionosphere, where the electric potential is hundreds of kilovolts higher than Earth's surface. It has not been clear, however, whether all the important components of the global circuit have even been identified. Here we report observations of five gigantic jets that establish a direct link between a thundercloud (altitude similar to16 km) and the ionosphere at 90 km elevation. Extremely-low-frequency radio waves in four events were detected, while no cloud-to-ground lightning was observed to trigger these events. Our result indicates that the extremely-low-frequency waves were generated by negative cloud-to-ionosphere discharges, which would reduce the electrical potential between ionosphere and ground. Therefore, the conventional picture of the global electric circuit needs to be modified to include the contributions of gigantic jets and possibly sprites(17,18).
  • M Sato, H Fukunishi, M Kikuchi, H Yamagishi, WA Lyons
    JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS 65 (5) 607 - 614 1364-6826 2003/03 [Refereed][Not invited]
     
    Waveform monitoring of ELF radio signals in the frequency range of 1-400 Hz have been carried out on a routine basis at Syowa station (69.0degreesS, 39.6degreesE in geographic coordinates), Antarctica since February, 2000. The main purpose of these observations is to monitor global lightning activity and to locate lightning-induced sprites and elves. The ELF observation system consisting of two search coil sensors (geomagnetic north south (H) and cast west (D) sensors) was installed at a remote unmanned observatory in West Ongul Island located 5 km southwest from Syowa station. As a back up system, the same system was installed near Syowa station in East Ongul Island. Signals from these sensors were digitally sampled at 1000 Hz with a GPS time code. On July 4, 2000 during the STEPS (Severe Thunderstorm Electrification and Precipitation Studies) 2000 campaign carried out over the Great Plains in the US, 57 sprite events were observed from Yucca Ridge Field Station (40.7degreesN, 104.9degreesW), Colorado, and 53 out of these sprite events had one-to-one correspondence to transient Schumann resonances (SR) detected at Syowa station. The waveforms of these SR are characterized by sharp initial pulses and following damped oscillations. The great circles representing the propagation paths are determined from the Lissojous plots of the H and D magnetic field data of the transient SR. It has been demonstrated that the minimum distance between the great circles and the locations of causative cloud-to-ground (CG) discharges is similar to240 km on average. It is thus concluded that the method to determine the propagation paths from Lissajous plots is extremely accurate when we use the Syowa ELF,waveform data. Consequently, it would be possible to globally triangulate sprite-inducing CG locations by setting up at least one more observation site with the same system. (C) 2003 Elsevier Science Ltd. All rights reserved.
  • N Sato, DM Wright, Y Ebihara, M Sato, Y Murata, H Doi, T Saemundsson, SE Milan, M Lester, CW Carlson
    GEOPHYSICAL RESEARCH LETTERS 29 (21) 2041  0094-8276 2002/11 [Refereed][Not invited]
     
    We have made a direct comparison of a pulsating aurora observed simultaneously from the ground at Syowa in Antarctica and onboard the FAST satellite (similar to3100 km altitude). The auroral form appeared as east-west-aligned bands consisting of two different types: a poleward moving pulsation and a standing mode pulsation, each with a period of similar to5 sec. The aurora occurs within the region of an inverted-V structure of lower energy (0.1-1 keV) electron precipitation. The two different types of pulsating aurora are separated in space by a narrow gap in the inverted-V potential structure. Spatial and temporal variations of the down-going high-energy (>5 keV) electron flux show a one-to-one correspondence with the optical pulsating aurora. The down-going high-energy (1-10 keV) ion flux modulation is out of phase (anti-correlated) with the high-energy electron flux modulation. These features suggest that the precipitating high-energy electrons, which produce the pulsating aurora, are modulated by the oscillation of the field-aligned electric field located above FAST.
  • Füllekrug, M, S. Constable, G. Heinson, M. Sato, Y. Takahashi, C. Price, E. Williams
    EOS 81 333  2000/07 [Refereed][Not invited]
  • M Sato, H Fukunishi, LJ Lanzerotti, CG Maclennan
    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 104 (A9) 19971 - 19982 0148-0227 1999/09 [Refereed][Not invited]
     
    Magnetic field data obtained by fluxgate and search coil magnetometers installed at four Automatic Geophysical Observatories (AGO P1, P2, P3, and P4) and at South Pole and McMurdo in Antarctica and at Iqaluit on Baffin Island are used to study the relationship between magnetic impulse events (MIEs) and Pc1 bursts at high geomagnetic latitudes. The spatial scale sizes of MIEs are determined in the investigation of the sources of these events in the magnetosphere. Four MIE events with simultaneous Pc1 bursts are studied. Contour plots of MIE amplitudes show the scale sizes of the examined MIEs to be 5 degrees to 7 degrees in the magnetic latitude direction and 40 degrees to 60 degrees in the magnetic longitude direction. Temporal changes of the ionospheric currents calculated from the fluxgate H- and D-component data indicate that the "convection vortices" associated with the MIEs traveled westward and decayed rapidly. An important finding is that MIE-related Pc1 bursts were observed at higher-latitude (P1, P4 near 80 degrees) and lower-latitude (P2, P3 near 70 degrees) AGO stations and South Pole Station at 74 degrees with different spectral structures, although the Pc1 spectral power was always a maximum at South Pole Station. These results imply that Pc1 bursts are excited not only in the dayside outer magnetosphere but also in the low-latitude boundary layer region.
  • Dayside auroral dynamics observed by the AGO network in Antarctica
    Sato, M, H. Fukunishi, R. Kataoka, A. Shono, L.J. Lanzerotti, J.H. Doolittle, S.B. Mende, M. Pinnock
    Adv. Polar Upp. Atmos. Res. 13 67 - 78 1999 [Refereed][Not invited]
  • H Fukunishi, Y Takahashi, M Sato, A Shono, M Fujito, Y Watanabe
    GEOPHYSICAL RESEARCH LETTERS 24 (23) 2973 - 2976 0094-8276 1997/12 [Refereed][Not invited]
     
    Optical and search coil magnetometer data obtained from the SPRITES'96 campaign carried out at Yucca Ridge Field Station, Colorado in July 1996 have presented clear evidence for the excitation of OLF transients with their dominant power at 1-2 Hz by strong lightning discharges producing elves and sprites. The most striking feature is that the ULF transients exhibit different wave forms in the case of sprites without, preceding elves and the case of sprites with preceding elves. In the former case damped, quasi-sinusoidal oscillations commence impulsively at the onset of sprites, while in; the latter case quasi-sinusoidal wavelets with a duration of similar to 3 s are excited. and elves and sprites occur within each wavelet. It is likely that these ULF transients are due to the nonlinear excitation of the ionospheric Alfven resonator by strong lightning discharge, as proposed by Sukhorukov and Stubbe [1997].

Books etc

  • 地球惑星科学入門 第2版
    在田 一則, 竹下 徹, 見延 庄士郎, 渡部 重十 (Joint work第34章 太陽と宇宙空間)
    北海道大学出版会 2015/03
  • 地球惑星科学入門
    在田 一則, 竹下 徹, 見延 庄士郎, 渡部 重十 (Joint work第34章 太陽と宇宙空間)
    北海道大学出版会 2010/10

Conference Activities & Talks

  • Relation between Lightning Activities Measured by the V-POTEKA Network and Intensity Development of 2018 Pacific Typhoons  [Not invited]
    Sato, M, Y. Takahashi, H. Kubota, K. Yamashita, J. Hamada, J.J. Marciano
    SGEPSS 146th Meeting  2019/10
  • Prediction of the typhoon intensity development by monitoring lightning activity  [Invited]
    Sato, M, Y. Takahashi, H. Kubota, K. Yamashita, J. Hamada, J.J. Marciano
    Asia Oceania Geosciences Society (AOGS) 16th Annual Meeting  2019/08
  • Relation between lightning and typhoon activities (Typhoon YAGI) in the western Pacific rsegion  [Not invited]
    Sato, M, Y. Takahashi, H. Kubota, K. Yamashita, J. Hamada, J.J. Marciano
    JpGU 2019 Meeting  2019/05
  • Relation between lightning and typhoon activities (typhoon LAN) in the western Pacific region  [Not invited]
    Sato, M, Y. Takahashi, H. Kubota, K. Yamashita, J. Hamada, J.J. Marciano
    EGU General Assembly 2019  2019/04
  • Relation between lightning and typhoon activities in the western Pacific region  [Not invited]
    Sato, M, Y. Takahashi, H. Kubota, K. Yamashita, J. Hamada, E. Momota, J.J. Marciano
    AGU Fall Meeting 2018  2018/12
  • Relation between Typhoon Intensity and Lightning Activity Measured by the V-POTEKA Network  [Not invited]
    Sato, M, Y. Takahashi, K. Yamashita, H. Kubota, J. Hamada, J. Hamada, J.J. Marciano
    SGEPSS 144th Meeting  2018/11
  • Future Lightning Observation from Spacecraft for the Identification of Planetary Atmospheric Convection Structure  [Not invited]
    Sato, M, Y. Takahashi, J, Haruyama, M. Imai
    The Meteorological Society of Japan 2018 Meeting  2018/10
  • Introduction of Hokkaido University and Research Activities in Department of Cosmosciences  [Invited]
    SATO Mitsuteru
    1st International conference on Applied Science, Engineering and Interdisciplinary Studies 2018  2018/07
  • Development of lightning observation network in the western Pacific region for the intensity prediction of severe weather and tropical cyclone  [Not invited]
    Sato, M, Y. Takahashi, H. Kubota, K. Yamashita, J. Hamada, J.J. Marciano
    16th International Conference on Atmospheric Electricity (ICAE)  2018/06
  • ULAT project: Lightning observations in the Philippines and western Pacific region for the intensity prediction of severe weather  [Invited]
    Sato, M, Y. Takahashi, H. Kubota, K. Yamashita, J. Hamada, J.J. Marciano
    Asia Oceania Geosciences Society (AOGS) 15th Annual Meeting  2018/06
  • Lightning observations in the Philippines and western Pacific region for the intensity prediction of severe weather  [Not invited]
    Sato, M, Y. Takahashi, H. Kubota, K. Yamashita, J. Hamada, J.J. Marciano
    JpGU 2018  2018/05
  • ULAT project: Lightning observations in the Philippines for the intensity prediction of severe weather  [Not invited]
    Sato, M, Y. Takahashi, K. Yamashita, H. Kubota, J. Hamada, J.J. Marciano
    EGU General Assembly 2018  2018/04
  • 宇宙空間からの雷放電光学・電波観測  [Not invited]
    佐藤 光輝
    「雷雲と宇宙線の相互作用に伴う高エネルギー現象」研究会  2018/03
  • Development of lightning observation network in the western Pacific region for the intensity prediction of severe weather  [Not invited]
    Sato, M, Y. Takahashi, K. Yamashita, H. Kubota, J. Hamada, E. Momota, J.J. Marciano
    AGU Fall Meeting 2017  2017/12
  • Construction of Lightning Observation Network in Asian Countries for the Intensity Development Prediction of Severe Weather  [Not invited]
    Mitsuteru SATO, Yukihiro Takahashi, Kozo Yamashita, Hisayuki Kubota, Junichi Hamada, Eriko Momota, Joel Marciano
    142nd SGEPSS meeting  2017/10
  • Optical and electromagnetic characteristics of lightning and TLEs derived from the JEM-GLIMS nadir observations  [Invited]
    Sato, M, H. Kikuchi, T. Ushio, T. Adachi, T. Sato, T. Morimoto, M. Suzuki, A. Yamazaki, Y. Takahashi
    32nd URSI General Assembly & Scientific Symposium  2017/08
  • Deployment Plan of ELF observation system in Asian countries to monitor severe weather development  [Not invited]
    Sato, M, Y. Takahashi, H. Kubota, C. Shimizu
    JpGU-AGU Meeting 2017  2017/05
  • Operation of lightning detection network and micro-satellites for nowcast of thunderstorm and tropical cyclone activities  [Not invited]
    Sato, M, Y. Takahashi, H. Kubota, E. Momota, J. Marciano
    EGU General Assembly 2017  2017/04
  • 北海道大学における地球惑星観測装置群の現状と課題  [Not invited]
    佐藤光輝
    名古屋大学宇宙地球環境研究所 研究集会「太陽地球系科学に於ける地上観測の現状と課題」  2017/03
  • Global occurrence rates and their LT/monthly/seasonal variations of lightning, elves, and sprites derived from JEM-GLIMS observations  [Not invited]
    Sato, M, T. Sato, T. Adachi, T. Ushio, T. Morimoto, M. Suzuki, A. Yamazaki, Y. Takahashi
    AGU Fall Meeting 2016  2016/12
  • Simulation of electron density inhomogeneity induced by sprite-producing lightning discharges  [Not invited]
    Mitsuteru SATO, Yasutaka Hiraki, Toru Adachi, Tomoo Ushio, Takeshi Morimoto, Hiroshi Kikuchi, Makoto Suzuki, Atsushi Yamazaki, Yukihiro Takahashi
    140th SGEPSS meeting  2016/11
  • Global occurrence rates of lightning, sprites, and elves and their LT dependences derived from JEM-GLIMS nadir observations  [Invited]
    Sato, M, T. Sato, T. Adachi, T. Ushio, T. Morimoto, H. Kikuchi, M. Suzuki, A. Yamazaki, Y. Takahashi, U. Inan, I. Linscott, Y. Hobara
    Asia Oceania Geosciences Society (AOGS) 12th Annual Meeting  2016/08
  • Future observations of lightning-exciting ELF waves in Asian region for the nowcasting of severe weather development  [Not invited]
    Sato, M, C. Shimizu, F. Tsuchiya, N. Honma, Y. Hongo, Y. Takahashi
    JpGU Meeting 2016  2016/05
  • Horizontal Distributions of Sprites and the Relation to Parent Lightning Discharges Derived from JEM-GLIMS Nadir Observations  [Not invited]
    Mitsuteru Sato, Toru Adachi, Tsuyoshi Sato, Tomoo Ushio, Takeshi Morimoto, Makoto Suzuki, Atsushi Yamazaki, Yukihiro Takahashi
    JpGU Meeting 2016  2016/05
  • Results from the GLIMS mission  [Invited]
    Mitsuteru Sato
    TEA-IS 2015 Workshop  2016/04
  • JEM-GLIMSによる3年間の雷放電・高高度放電発光現象観測結果  [Not invited]
    佐藤光輝, 牛尾知雄, 森本健志, 佐藤剛志, 足立透, 菊池博史, 鈴木睦, 山崎敦, 高橋幸弘, Umran Inan, Ivan Linscott, 芳原容英
    第16回宇宙科学シンポジウム  2016/01
  • An overview of three-year JEM-GLIMS nadir observations of lightning and TLEs  [Invited]
    Sato, M, T. Ushio, T. Morimoto, T. Sato, T. Adachi, H. Kikuchi, M. Suzuki, A. Yamazaki, Y. Takahashi, U. Inan, I. Linscott, Y. Hobara
    AGU Fall Meeting 2015  2015/12
  • JEM-GLIMSによる3年間の雷放電・高高度 放電発光現象の観測成果  [Not invited]
    佐藤光輝, 牛尾知雄, 森本健志, 足立透, 菊池博史, 鈴木睦, 山崎敦, 高橋幸弘, Ivan Linscott, Umran Inan, 芳原容英
    第138回地球電磁気・地球惑星圏学会  2015/10
  • 全球雷活動の周期的変動と地球気候変動および太陽活動との関係  [Not invited]
    佐藤光輝, 高橋幸弘, 鴨川仁
    第138回地球電磁気・地球惑星圏学会  2015/10
  • 電磁波・大気電場観測が明らかにする全球雷活動と大気変動  [Not invited]
    佐藤光輝, 鴨川仁, 高橋幸弘, 源泰拓, 門倉昭
    第7回極域観測シンポジウム  2015/09
  • 2.5-years of observations of lightning and TLEs by JEM-GLIMS from the ISS  [Invited]
    Sato, M, T. Ushio, T. Morimoto, M. Mihara, T. Sato, C. Shimizu, T. Adachi, H. Kikuchi, M. Suzuki, A. Yamazaki, Y. Takahashi
    Asia Oceania Geosciences Society (AOGS) 12th Annual Meeting  2015/08
  • 2.5-years of observations of lightning and TLEs by JEM-GLIMS  [Not invited]
    Sato, M, T. Ushio, T. Morimoto, M. Mihara, T. Sato, C. Shimizu, T. Adachi, H. Kikuchi, M. Suzuki, A. Yamazaki, Y. Takahashi
    26th IUGG General Assembly 2015  2015/06
  • 静止軌道からの雷放電観測の重要性  [Not invited]
    佐藤光輝, 牛尾知雄, 足立透, 鈴木睦
    日本地球惑星科学連合2015年大会  2015/05
  • JEM-GLIMS光学観測データから推定した雷放電・TLEsの全球発生頻度分布  [Not invited]
    佐藤光輝, 佐藤剛志, 三原正大, 清水千春, 足立透, 牛尾知雄, 森本健志, 鈴木睦, 山崎敦, 高橋幸弘
    日本地球惑星科学連合2015年大会  2015/05
  • Relation between sprite distribution and source locations of VHF pulses derived from JEM-GLIMS measurements  [Invited]
    Sato, M, M. Mihara, T. Ushio, T. Morimoto, H. Kikuchi, T. Adachi, M. Suzuki, A. Yamazaki, Y. Takahashi
    EGU General Assembly 2015  2015/04

MISC

  • R. Kitamura, Y. Hobara, M. Sato, Y. Takahashi, T. Adachi, T. Ushio, M. Suzuki  2019 URSI Asia-Pacific Radio Science Conference, AP-RASC 2019  2019/03  [Not refereed][Not invited]
     
    © 2019 URSI. All rights reserved. Recent study by [1] demonstrates the remarkable similarity between the time series of lightning optical irradiance observed by high speed photometric observations in GLIMS (Global LIghtning and sprite MeasurementS on JEMEF) mission installed in the International Space Station (ISS) and current moment change estimated by groundbased ELF magnetic field measurement based on 169 lightning strokes around Japan, which also indicates the high correlation between integrated irradiance and charge moment change (Qds).
  • ISHIGURO Masateru, GEEM Jooyeon, NAITO Hiroyuki, BACH Yoonsoo P, KURODA Daisuke, ONO Tatsuharu, TAKAGI Seiko, SATO Mitsuteru, KURAMOTO Kiyoshi, SEKIGUCHI Tomohiko, IMAI Masataka, WATANABE Makoto, OHTSUKA Katsuhito, HASEGAWA Sunao, ITO Takashi, YOSHIDA Fumi, ARAI Tomoko  日本地球惑星科学連合大会予稿集(Web)  2019-  ROMBUNNO.PPS03‐P17 (WEB ONLY)  2019  [Not refereed][Not invited]
  • 和田有希, 和田有希, 榎戸輝揚, 松元崇弘, 中澤知洋, 古田禄大, 湯浅孝行, 土屋晴文, 米徳大輔, 澤野達哉, 牧島一夫, 牧島一夫, 鴨川仁, 中村佳敬, 森本健志, 佐藤光輝, 酒井英男, 南戸秀仁, 牛尾知雄  日本地球惑星科学連合大会予稿集(Web)  2019-  ROMBUNNO.MIS27‐10 (WEB ONLY)  2019  [Not refereed][Not invited]
  • GEEM Jooyeon, ISHIGURO Masateru, BACH Yoonsoo P, KURODA Daisuke, NAITO Hiroyuki, HANAYAMA Hidekazu, KIM Yoonyoung, KWON Yuna G, JIN Sunho, SEKIGUCHI Tomohiko, OKAZAKI Ryo, VAUBAILLON Jeremie J, IMAI Masataka, OONO Tatsuharu, FUTAMUTS Yuki, TAKAGI Seiko, SATO Mitsuteru, KURAMOTO Kiyoshi, WATANABE Makoto  日本地球惑星科学連合大会予稿集(Web)  2019-  ROMBUNNO.PPS03‐P04 (WEB ONLY)  2019  [Not refereed][Not invited]
  • Yukihiro Takahashi, Mitsuteru Sato, Masataka Imai, Ralph Lorenz, Yoav Yair, Karen Aplin, Georg Fischer, Masato Nakamura, Nobuaki Ishii, Takumi Abe, Takumi Abe, Takehiko Satoh, Takehiko Satoh, Takeshi Imamura, Chikako Hirose, Makoto Suzuki, George L. Hashimoto, Naru Hirata, Atsushi Yamazaki, Atsushi Yamazaki, Takao M. Sato, Manabu Yamada, Shin ya Murakami, Yukio Yamamoto, Tetsuya Fukuhara, Kazunori Ogohara, Hiroki Ando, Ko ichiro Sugiyama, Hiroki Kashimura, Shoko Ohtsuki  Earth, Planets and Space  70-  2018/12/01  [Not refereed][Not invited]
     
    © 2018, The Author(s). The existence of lightning discharges in the Venus atmosphere has been controversial for more than 30 years, with many positive and negative reports published. The lightning and airglow camera (LAC) onboard the Venus orbiter, Akatsuki, was designed to observe the light curve of possible flashes at a sufficiently high sampling rate to discriminate lightning from other sources and can thereby perform a more definitive search for optical emissions. Akatsuki arrived at Venus during December 2016, 5 years following its launch. The initial operations of LAC through November 2016 have included a progressive increase in the high voltage applied to the avalanche photodiode detector. LAC began lightning survey observations in December 2016. It was confirmed that the operational high voltage was achieved and that the triggering system functions correctly. LAC lightning search observations are planned to continue for several years.
  • 榎戸輝揚, 和田有希, 和田有希, 古田禄大, 中澤知洋, 湯浅孝行, 奥田和史, 牧島一夫, 佐藤光輝, 佐藤陽祐, 中野俊男, 楳本大悟, 土屋晴文, 土屋晴文  日本物理学会講演概要集(CD-ROM)  73-  (1)  ROMBUNNO.22pK305‐7  2018/03/23  [Not refereed][Not invited]
  • 和田有希, 和田有希, 古田禄大, 榎戸輝揚, 中澤知洋, 中澤知洋, 湯浅孝行, 奥田和史, 牧島一夫, 佐藤光輝, 佐藤陽祐, 中野俊男, 楳本大悟, 土屋晴文  日本物理学会講演概要集(CD-ROM)  73-  (1)  ROMBUNNO.22aK308‐7  2018/03/23  [Not refereed][Not invited]
  • 古田禄大, 和田有希, 和田有希, 榎戸輝揚, 中澤知洋, 湯浅孝行, 奥田和史, 牧島一夫, 佐藤光輝, 佐藤陽祐, 中野俊男, 楳本大悟, 土屋晴文  日本物理学会講演概要集(CD-ROM)  73-  (1)  ROMBUNNO.22aK308‐8  2018/03/23  [Not refereed][Not invited]
  • 高橋 幸弘, 今井 正尭, 佐藤 光輝  遊・星・人 = Planetary people : 日本惑星科学会誌  27-  (1)  43  -45  2018/03  [Not refereed][Not invited]
  • 中澤知洋, 榎戸輝揚, 和田有希, 和田有希, 古田禄大, 松元崇弘, 春日知明, 奥田和史, 湯浅孝行, 中野俊男, 楳本大悟, 加藤博, 牧島一夫, 佐藤光輝, 佐藤陽祐, 土屋晴文  日本天文学会年会講演予稿集  2018-  240  2018/02/20  [Not refereed][Not invited]
  • 鈴木克徳, 柿沼遠方, 芳原容英, 佐藤光輝, 高橋幸弘, 足立透, 牛尾知雄, 河崎善一郎, 森本健志, 山崎敦, 鈴木睦, LINSCOTT I. R, INAN U. S  大気電気学会誌  11-  (1)  102‐103  2017/11/15  [Not refereed][Not invited]
  • 清水千春, 佐藤光輝, 高橋幸弘, 本郷保二, 土屋史紀, 阿部修司, 吉川顕正  大気電気学会誌  11-  (1)  59‐60  2017/11/15  [Not refereed][Not invited]
  • G. Abdellaoui, S. Abe, A. Acheli, J. H. J. H. Adams, S. Ahmad, A. Ahriche, J. -N. Albert, D. Allard, G. Alonso, L. Anchordoqui, V. Andreev, A. Anzalone, W. Aouimeure, Y. Arai, N. Arsene, K. Asano, R. Attallah, H. Attoui, M. Ave Pemas, S. Bacholle, M. Bakiri, P. Baragatti, P. Barrillon, S. Bartocci, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, A. Belov, K. Belov, B. Benadda, K. Benmessai, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, F. Bisconti, N. Blanc, J. Blecki, S. Blin-Bondil, P. Bobik, M. Bogomilov, M. Bonamente, R. Boudaoud, E. Bozzo, M. S. Briggs, A. Bruno, K. S. Caballero, F. Cafagna, D. Campana, J. -N. Capdevielle, F. Capel, A. Caramete, L. Caramete, P. Carlson, R. Caruso, M. Casolino, C. Cassardo, A. Castellina, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, G. Chiritoi, M. J. Christl, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, M. Di Martino, T. Djemil, S. A. Djenas, F. Dulucq, M. Dupieux, I. Dutan, A. Ebersoldt, T. Ebisuzaki, R. Engel, J. Eser, K. Fang, F. Fenu, S. Fernandez-Gonzalez, J. Fernandez-Soriano, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, M. Fouka, A. Franceschi, S. Franchini, C. Fuglesang, J. Fujimoto, M. Fukushima, P. Galeotti, E. Garcia-Ortega, G. Garipov, E. Gascon, J. Geary, G. Gelmini, J. Genci, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, R. Guehaz, A. Guzman, Y. Hachisu, M. Haiduc, B. Harlov, A. Haungs, J. Hernandez Carretero, W. Hidber, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, F. Isgro, Y. Itow, T. Jammer, E. Joven, E. G. Judd, A. Jung, J. Jochum, F. Kajino, T. Kajino, S. Kalli, I. Kaneko, D. Kang, F. Kanouni, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, A. Kedadra, H. Khales, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, H. Lahmar, F. Lakhdari, O. Larsson, J. Lee, J. Licandro, H. Lim, L. Lopez Campano, M. C. Maccarone, S. Mackovjak, M. Mandi, D. Maravilla, L. Marcelli, J. L. Marcos, A. Marini, K. Martens, Y. Martin, O. Martinez, G. Masciantonio, K. Mase, R. Matev, J. N. Matthews, N. Mebarki, G. Medina-Tanco, L. Mehrad, M. A. Mendoza, A. Merino, T. Memik, J. Meseguer, S. Messaoud, O. Micu, J. Mimouni, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, B. Nadji, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, A. Nardellis, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleariski, G. Osteria, W. Painter, M. I. Panasyuk, B. Panico, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, M. Perdichizzi, I. Perez-Grande, F. Perfetto, T. Peter, P. Picozza, T. Pierog, S. Pindado, L. W. Piotrowski, S. Pirainou, L. Placidis, Z. Plebaniak, S. Pliego, A. Pollini, E. M. Popescu, P. Prat, G. Prevot, H. Prieto, M. Putis, J. Rabanal, A. A. Radu, M. Rahmani, P. Reardon, M. Reyes, M. Rezazadeh, M. Ricci, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, Z. Sahnoune, A. Saito, N. Sakaki, M. Sakata, H. Salazar, J. C. Sanchez, J. L. Sanchez, A. Santangelo, L. Santiago Cruz, A. Sanz-Andres, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, J. Sledd, K. Slomiriska, A. Sobey, I. Stan, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, H. Tahi, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, M. C. Talai, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, M. Traiche, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, G. Vankova, C. Vigorito, L. Villasenor, B. Vicek, P. von Ballmoos, M. Vrabel, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, R. Weigand Munoz, A. Weindl, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, S. Yoshida, R. Young, I. S. Zgura, M. Yu. Zotov, A. Zuccaro Marchi  PLANETARY AND SPACE SCIENCE  143-  245  -255  2017/09  [Not refereed][Not invited]
     
    We summarize the state of the art of a program of UV observations from space of meteor phenomena, a secondary objective of the JEM-EUSO international collaboration. Our preliminary analysis indicates that JEM-EUSO, taking advantage of its large FOV and good sensitivity, should be able to detect meteors down to absolute magnitude close to 7. This means that JEM-EUSO should be able to record a statistically significant flux of meteors, including both sporadic ones, and events produced by different meteor streams. Being unaffected by adverse weather conditions, JEM-EUSO can also be a very important facility for the detection of bright meteors and fireballs, as these events can be detected even in conditions of very high sky background. In the case of bright events, moreover, exhibiting some persistence of the meteor train, preliminary simulations show that it should be possible to exploit the motion of the ISS itself and derive at least a rough 3D reconstruction of the meteor trajectory. Moreover, the observing strategy developed to detect meteors may also be applied to the detection of nuclearites, exotic particles whose existence has been suggested by some theoretical investigations. Nuclearites are expected to move at higher velocities than meteoroids, and to exhibit a wider range of possible trajectories, including particles moving upward after crossing the Earth. Some pilot studies, including the approved Mini-EUSO mission, a precursor of JEM-EUSO, are currently operational or in preparation. We are doing simulations to assess the performance of Mini-EUSO for meteor studies, while a few meteor events have been already detected using the ground-based facility EUSO-TA.
  • G. Abdellaoui, S. Abe, A. Acheli, J. H. Adams, S. Ahmad, A. Ahriche, J. -N. Albert, D. Allard, G. Alonso, L. Anchordoqui, V. Andreev, A. Anzalone, W. Aouimeur, Y. Arai, N. Arsene, K. Asano, R. Attallah, H. Attoui, M. Ave Pernas, S. Bacholle, M. Bakiri, P. Baragatti, P. Barrillon, S. Bartocci, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, A. Belov, K. Belov, B. Benadda, K. Benmessai, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, F. Bisconti, N. Blanc, J. Blecki, S. Blin-Bondil, P. Bobik, M. Bogomilov, M. Bonamente, R. Boudaoud, E. Bozzo, M. S. Briggs, A. Bruno, K. S. Caballero, F. Cafagna, D. Campana, J. -N. Capdevielle, F. Capel, A. Caramete, L. Caramete, P. Carlson, R. Caruso, M. Casolino, C. Cassardo, A. Castellina, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, G. Chiritoi, M. J. Christl, V. Connaughton, L. Conti, G. Contino, G. Cordero, G. Cotto, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, M. Di Martino, T. Djemil, S. A. Djenas, F. Dulucq, M. Dupieux, I. Dutan, A. Ebersoldt, T. Ebisuzaki, R. Engel, J. Eser, K. Fang, F. Fenu, S. Fernandez-Gonzalez, J. Fernandez-Soriano, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, R. Forza, M. Fouka, A. Franceschi, S. Franchini, C. Fuglesang, J. Fujimoto, M. Fukushima, P. Galeotti, E. Garcia-Ortega, G. Garipov, E. Gascon, J. Geary, G. Gelmini, J. Genci, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, N. Guardone, F. Guarino, R. Guehaz, A. Guzman, Y. Hachisu, M. Haiduc, B. Harlov, A. Haungs, J. Hernandez Carretero, W. Hidber, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, T. Jammer, E. Joven, E. G. Judd, A. Jung, J. Jochum, F. Kajino, T. Kajino, S. Kalli, I. Kaneko, D. Kang, F. Kanouni, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, A. Kedadra, H. Khales, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, H. Lahmar, F. Lakhdari, O. Larsson, J. Lee, J. Licandro, H. Lim, L. Lopez Campano, M. C. Maccarone, S. Mackovjak, M. Mahdi, M. Manfrin, D. Maravilla, L. Marcelli, J. L. Marcos, A. Marini, K. Martens, Y. Martin, O. Martinez, G. Masciantonio, K. Mase, R. Matev, J. N. Matthews, N. Mebarki, G. Medina-Tanco, L. Mehrad, M. A. Mendoza, A. Merino, T. Mernik, J. Meseguer, S. Messaoud, O. Micu, M. Mignone, J. Mimouni, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, B. Nadji, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, W. Painter, M. I. Panasyuk, B. Panico, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, I. Perez-Grande, F. Perfetto, T. Peter, P. Picozza, T. Pierog, S. Pindado, L. W. Piotrowski, S. Piraino, L. Placidi, Z. Plebaniak, S. Pliego, A. Pollini, E. M. Popescu, P. Prat, G. Prevot, H. Prieto, M. Putis, J. Rabanal, A. A. Radu, M. Rahmani, P. Reardon, M. Reyes, M. Rezazadeh, M. Ricci, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, Z. Sahnoune, A. Saito, N. Sakaki, M. Sakata, H. Salazar, J. C. Sanchez, J. L. Sanchez, A. Santangelo, L. Santiago Cruz, A. Sanz-Andres, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, J. Sledd, K. Slominska, A. Sobey, I. Stan, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, H. Tahi, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, M. C. Talai, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, M. Traiche, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, G. Vankova, C. Vigorito, L. Villasenor, B. Vlcek, P. von Ballmoos, M. Vrabel, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, R. Weigand Munoz, A. Weindl, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, S. Yoshida, R. Young, I. S. Zgura, M. Yu. Zotov, A. Zuccaro Marchi  NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT  866-  150  -163  2017/09  [Not refereed][Not invited]
     
    JEM-EUSO is a space mission designed to investigate Ultra-High Energy Cosmic Rays and Neutrinos (E > 5.10(19) eV) from the International Space Station (ISS). Looking down from above its wide angle telescope is able to observe their air showers and collect such data from a very wide area. Highly specific trigger algorithms are needed to drastically reduce the data load in the presence of both atmospheric and human activity related background light, yet retain the rare cosmic ray events recorded in the telescope. We report the performance in offline testing of the first level trigger algorithm on data from JEM-EUSO prototypes and laboratory measurements observing different light sources: data taken during a high altitude balloon flight over Canada, laser pulses observed from the ground traversing the real atmosphere, and model landscapes reproducing realistic aspect ratios and light conditions as would be seen from the ISS itself. The first level trigger logic successfully kept the trigger rate within the permissible bounds when challenged with artificially produced as well as naturally encountered night sky background fluctuations and while retaining events with general air-shower characteristics. (C) 2017 Elsevier B.V. All rights reserved.
  • 芳原容英, 鈴木克徳, 柿沼遠方, 佐藤光輝, 高橋幸弘, 足立透, 牛尾知雄, 河崎善一郎, 森本健志, 山崎敦, 鈴木睦, LINSCOTT Ivan, INAN Umran  日本地球惑星科学連合大会予稿集(Web)  2017-  ROMBUNNO.MIS05‐06 (WEB ONLY)  2017  [Not refereed][Not invited]
  • BANDHOLNOPPARAT Kittanapat, SATO Mitsuteru, TAKAHASHI Yukihiro, ADACHI Toru, USHIO Tomoo  日本地球惑星科学連合大会予稿集(Web)  2017-  ROMBUNNO.MIS05‐P03 (WEB ONLY)  2017  [Not refereed][Not invited]
  • USHIO Tomoo, SATO Mitsuteru, KIKUCHI Hiroshi, MEGA Tomoaki, YOSHIKAWA Eiichi, NAKAMURA Yoshitaka  日本地球惑星科学連合大会予稿集(Web)  2017-  ROMBUNNO.ACG49‐02 (WEB ONLY)  2017  [Not refereed][Not invited]
  • Takeshi Morimoto, Hiroshi Kikuchi, Mitsuteru Sato, Tomoo Ushio, Atsushi Yamazaki, Makoto Suzuki, Ryohei Ishida, Yuji Sakamoto, Kazuya Yoshida, Yasuhide Hobara, Takuki Sano, Takumi Abe, Zen Ichiro Kawasaki  Earth, Planets and Space  68-  (1)  2016/12/01  [Not refereed][Not invited]
     
    © 2016 The Author(s). The Global Lightning and sprIte MeasurementS (GLIMS) mission has been conducted at the Exposed Facility of Japanese Experiment Module (JEM-EF) of the International Space Station for more than 30 months. This paper focuses on an electromagnetic (EM) payload of JEM-GLIMS mission, the very high frequency (VHF) broadband digital InTerFerometer (VITF). The JEM-GLIMS mission is designed to conduct comprehensive observations with both EM and optical payloads for lightning activities and related transient luminous events. Its nominal operation continued from November 2012 to December 2014. The extended operation followed for eight months. Through the operation period, the VITF collected more than two million VHF EM waveforms in almost 18,700 datasets. The number of VITF observations synchronized with optical signal is 8049. Active VHF radiations are detected in about 70 % of optical observations without obvious regional or seasonal dependency. Estimations of the EM direction-of-arrival (DOA) are attempted using the broadband digital interferometry. Some results agree with the optical observations, even though DOA estimation is problematic because of a very short antenna baseline and multiple pulses over a short time period, namely burst-type EM waveforms. The world's first lightning observations by means of space-borne VHF interferometry are achieved in this mission. This paper summarizes VITF instruments, the recorded VHF EM signals, and the results of DOA estimations by means of digital interferometry as a preliminary report after termination of the mission.
  • 森本健志, 菊池博史, 牛尾知雄, 佐藤光輝, 山崎敦, 鈴木睦, 菊池雅行  日本気象学会大会講演予稿集  (109)  350  2016/04/30  [Not refereed][Not invited]
  • 柿沼遠方, 芳原容英, 牛尾知雄, 河崎善一郎, 森本健志, 佐藤光輝, 山崎敦, 鈴木睦  大気電気学会誌  10-  (1)  52‐53  2016/04/10  [Not refereed][Not invited]
  • 一番星へ行こう! 日本の金星探査機の挑戦その29 〜巨大な弓形雲頂温度構造の発見〜
    田口真, 福原哲哉, 今村剛, 神山徹, 二口将彦, はしもとじょーじ, 鈴木睦, 上野宗孝, 岩上直幹, 佐藤隆雄, 佐藤光輝, 高木聖子, 中村正人  日本惑星科学会誌「遊星人」  25-  (4)  2  -16  2016  [Not refereed][Not invited]
  • 佐藤光輝, 足立透, 佐藤剛志, 牛尾知雄, 森本健志, 鈴木睦, 山崎敦, 高橋幸弘  日本地球惑星科学連合大会予稿集(Web)  2016-  ROMBUNNO.PEM16‐12 (WEB ONLY)  2016  [Not refereed][Not invited]
  • 佐藤剛志, 佐藤光輝, 牛尾知雄, 森本健志, 足立透, 鈴木睦, 山崎敦, 高橋幸弘  日本地球惑星科学連合大会予稿集(Web)  2016-  ROMBUNNO.PEM16‐P04 (WEB ONLY)  2016  [Not refereed][Not invited]
  • 佐藤光輝, 平木康隆, 足立透, 牛尾知雄, 森本健志, 菊池博史, 鈴木睦, 山崎敦, 高橋幸弘  地球電磁気・地球惑星圏学会総会及び講演会(Web)  140th-  ROMBUNNO.R005‐P18 (WEB ONLY)  2016  [Not refereed][Not invited]
  • SHIMIZU Chiharu, SATO Mitsuteru, TAKAHASHI Yukihiro, TSUCHIYA Fuminori, HONGO Yasuji, ABE Shuji, YOSHIKAWA Akimasa  地球電磁気・地球惑星圏学会総会及び講演会(Web)  140th-  ROMBUNNO.R005‐P02 (WEB ONLY)  2016  [Not refereed][Not invited]
  • 牛尾知雄, 佐藤光輝, 鈴木睦, 森本健志, 菊池博史, 菊池雅行, 足立透, 山崎敦, 高橋幸弘, INAN U, LINSCOTT I, 石田良平, 坂本祐二, 吉田和哉, 芳原容英, 阿部琢己, 中村正人, 織田裕久  日本気象学会大会講演予稿集  (108)  380  2015/09/30  [Not refereed][Not invited]
  • 柿沼遠方, 芳原容英, 牛尾知雄, 河崎善一郎, 森本健志, 佐藤光輝, 山崎敦, 鈴木睦  大気電気学会誌  9-  (1)  132  -133  2015/04/20  [Not refereed][Not invited]
  • 鈴木克徳, 柿沼遠方, 芳原容英, LINSCOTT I.R, INAN U.S, 佐藤光輝, 高橋幸弘, 牛尾知雄, 河崎善一郎, 森本健志, 山崎敦, 鈴木睦  大気電気学会誌  9-  (1)  92  -93  2015/04/20  [Not refereed][Not invited]
  • 鈴木克徳, 柿沼遠方, 芳原容英, LINSCOTT Ivan, INAN Umran, 佐藤光輝, 高橋幸弘, 牛尾知雄, 河崎善一郎, 森本健志, 山崎敦, 鈴木睦  日本地球惑星科学連合大会予稿集(Web)  2015-  ROMBUNNO.PEM11‐12 (WEB ONLY)  2015  [Not refereed][Not invited]
  • 清水千春, 佐藤光輝, 高橋幸弘, 土屋史紀, 本間規泰, 本郷保二, 阿部修司, 吉川顕正  日本地球惑星科学連合大会予稿集(Web)  2015-  ROMBUNNO.MIS29‐07 (WEB ONLY)  2015  [Not refereed][Not invited]
  • 菊池博史, 森本健志, 牛尾知雄, 佐藤光輝, 山崎敦, 鈴木睦  電子情報通信学会技術研究報告  114-  (381(EMCJ2014 74-83))  53  -56  2014/12/12  [Not refereed][Not invited]
  • 石丸 亮, 坂本 祐二, 小林 正規, 郷内 稔也, 藤田 伸哉, 千秋 博紀, 和田 浩二, 石橋 高, 黒澤 耕介, 山田 学, 阿部 新助, 吉田 和哉, 佐藤 光輝, 高橋 幸弘, 松井 孝典  日本惑星科学会秋期講演会予稿集  2014-  "O13  -03"  2014/09/10  [Not refereed][Not invited]
  • 春山 純一, 高橋 幸弘, 佐藤 光輝  日本惑星科学会秋期講演会予稿集  2014-  "P2  -31"  2014/09/10  [Not refereed][Not invited]
  • 菊池博史, 森本健志, 牛尾知雄, 佐藤光輝, 山崎敦, 鈴木睦  電気学会基礎・材料・共通部門大会講演論文集(CD-ROM)  2014-  ROMBUNNO.21-A-A1-6  2014/08/21  [Not refereed][Not invited]
  • 佐藤光輝, 三原正大, 高橋幸弘, 足立透, 牛尾知尾, 森本健志, 鈴木睦, 山崎敦, 菊池雅行, INAN U, LINSCOTT I  大気電気学会誌  8-  (1)  37  2014/04/18  [Not refereed][Not invited]
  • 菊池博史, 森本健志, 牛尾知雄, 佐藤光輝, 山崎敦, 鈴木睦  大気電気学会誌  8-  (1)  143  -144  2014/04/18  [Not refereed][Not invited]
  • 柿沼遠方, 芳原容英, 牛尾知雄, 河崎善一郎, 森本健志, 佐藤光輝, 山崎敦, 鈴木睦  大気電気学会誌  8-  (1)  145  -146  2014/04/18  [Not refereed][Not invited]
  • 菊池博史, 森本健志, 吉田智, 牛尾知雄, 佐藤光輝, 鈴木睦  日本気象学会大会講演予稿集  (104)  281  2013/10/31  [Not refereed][Not invited]
  • 森本健志, 菊池博史, 吉田智, 牛尾知雄, 河崎善一郎, 佐藤光輝, 山崎敦, 鈴木睦  大気電気学会誌  7-  (2)  91  -92  2013/10/25  [Not refereed][Not invited]
  • KIKUCHI Hiroshi, MORIMOTO Takeshi, YOSHIDA Satoru, USHIO Tomoo, KAWASAKI Zen-Ichiro, SATO Mitsuteru, SUZUKI Makoto  電気学会研究会資料. EMC, 電磁環境研究会  2013-  (19)  35  -38  2013/06/21  [Not refereed][Not invited]
  • 菊池 博史, 吉田 智, 森本 健志, 牛尾 知雄, 河崎 善一郎, 佐藤 光輝, 鈴木 睦  大気電気学会誌 = / Society of Atmospheric Electricity of Japan  7-  (1)  89  -90  2013/04/26  [Not refereed][Not invited]
  • 佐藤光輝, 牛尾知雄, 森本健志, 足立透, 鈴木睦, 山崎敦, 菊池雅行, 高橋幸弘, INAN Umran, LINSCOTT Ivan, 芳原容英  大気圏シンポジウム・講演集(Web)  27th-  III-4 (WEB ONLY)  2013  [Not refereed][Not invited]
  • 菊池博史, 森本健志, 牛尾知雄, 佐藤光輝, 山崎敦, 鈴木睦, 菊池雅行, 高橋幸弘, 坂本祐二  地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM)  134th-  ROMBUNNO.S001-08  2013  [Not refereed][Not invited]
  • 佐藤光輝, 足立透, 牛尾知雄, 森本健志, 鈴木睦, 山崎敦, 菊池雅行, 高橋幸弘, INAN Umran, LINSCOTT Ivan, 芳原容英  地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM)  134th-  ROMBUNNO.S001-07  2013  [Not refereed][Not invited]
  • 牛尾 知雄, 森本 健志, 佐藤 光輝, 鈴木 睦, 山崎 敦, 芳原 容英, 菊地 雅行, 高橋 幸弘, INAN Umran, 石田 良平, 坂本 祐二, 吉田 和哉, 阿部 琢美, 河崎 善一郎  大気電気学会誌 = / Society of Atmospheric Electricity of Japan  6-  (2)  2012/11/15  [Not refereed][Not invited]
  • TAKAHASHI Y, SATO M, FUKUHARA T, KURIHARA J, NAKAJIMA K  Planetary People  21-  (3)  224  -228  2012/09/25  [Not refereed][Not invited]
     
    近年,木星大気の大規模構造を決める力学や,大気組成を決める化学過程を理解する上で,積乱雲や雷放電観測の重要性が指摘されている.しかし,対流強度は雲頂高度など雲本体の観測のみからでは難しい.雷放電発光の強度,頻度,高度の情報はそれを補う優れた指標のひとつであるが,通常のカメラでは時間分解能が不十分で,積乱雲活動の定量的な評価は困難である.ここで提案する雷放電発光検出器"OLD"は,高速撮像・画像処理によって雷放電発光の頻度から対流活動強度を求め,また色情報から高度推定することを可能にする.
  • ISHIDA Ryohei, SATO Mitsuteru, USHIO Tomoo, SUZUKI Makoto, MORIMOTO Takeshi, SAKAMOTO Yuji  The Proceedings of the Space Engineering Conference  2010-  (0)  _F1  -1_-_F1-4_  2011  [Not refereed][Not invited]
     
    In this report, we describe the outline of the GLIMS equipment equipped with the JEM exposed facility and the development of the equipment as an engineer belonging to the department of mechanical engineering of the university. Especially, we developed the equipment by the cooperation of Department of Science and Department of Engineering in the development of this mission equipment without ordering to the specialty company of the space appliance. We describe how the teacher at the university that is involved in mechanical engineering should be related to development so that Department of Science may cooperate with Department of Engineering.
  • NISHIYAMA Takanori, SAKANOI Takeshi, MIYOSHI Yoshizumi, KATAOKA Ryuho, ASAMURA Kazushi, SATO Mitsuteru, OKANO Shoichi  地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD−ROM)  130th-  ROMBUNNO.B006-P003  2011  [Not refereed][Not invited]
  • Tomoo Ushio, Mitsuteru Sato, Takeshi Morimoto, Makoto Suzuki, Hiroshi Kikuchi, Atsushi Yamazaki, Yukihiro Takahashi, Yasuhide Hobara, Umran Inan, Ivan Linscott, Yuji Sakamoto, Ryohei Ishida, Masavuki Kikuchi, Kazuya Yoshida, Zen Ichiro Kawasaki  IEEJ Transactions on Fundamentals and Materials  131-  (1)  16  -20  2011  [Not refereed][Not invited]
     
    Lightning and sprite measurement sensors on the International Space Station (ISS) are introduced in this paper. Lightning is an electrical discharge which neutralizes the charge inside thunderstorm. In the early 1990s, optical transient luminous events (TLEs) occurring just above the thunderstorm were firstly reported by the US scientists and are associated with positive cloud-to-ground discharges with a large amount of charge. Though the luminous events so-called sprite, elves and jets have been investigated by numerous researchers all over the world based mainly on the ground observations, some important problems have not been fully understood yet such as generation mechanisms of columniform fine structure and horizontal offset of some sprites from the parent lightning discharges. In the JEM-GLIMS mission, observations from our synchronized sensors are going to shed light on above-mentioned unsolved problems regarding TLEs as well as causative lighting discharges. Our goals are (1) to detect and locate lightning and sprite within storm scale resolution over a large region of the Earth's surface along the orbital track of the ISS without any bias, (2) to clarify the generation mechanism of sprite, and (3) to identify the occurrence conditions of TLEs. © 2011 The Institute of Electrical Engineers of Japan.
  • USHIO Tomoo, SATO Mitsuteru, MORIMOTO Takeshi, SUZUKI Makoto, KIKUCHI Hiroshi, YAMAZAKI Atsushi, TAKAHASHI Yukihiro, HOBARA Yasuhide, INAN Umran, ISHIDA Ryohei, KAWASAKI Zen-Ichiro  電気学会研究会資料. EMC, 電磁環境研究会  2010-  (29)  1  -4  2010/11/01  [Not refereed][Not invited]
  • SATO Mitsuteru, USHIO Tomoo, ISHIDA Ryohei, SUZUKI Makoto, MORIMOTO Takeshi, SAKAMOTO Yuji  The Proceedings of the Space Engineering Conference  2009-  (0)  97  -101  2010  [Not refereed][Not invited]
     
    In order to study the generation mechanism of lightning-associated transient luminous events (TLEs) and the relationship between lightning and TLEs, we will carry out the lightning and TLE observation at Exposed Facility of Japanese Experiment Module (JEM-EF) of International Space Station (ISS). In this mission named JEM-GLIMS (Global Lightning and sprlte MeasurementS on JEM-EF) two kinds of optical instruments and two sets of radio receivers will be integrated into the Multi mission Consolidated Equipment (MCE) which is the bus system and will be installed at JEM-EF finally. For the development of the GLIMS instruments, mechanical FEM analysis and thermal analysis are the important tasks to be performed by the mission team. Science group of the GLIMS mission has contacted to professors who belong to the department of engineering in an university and are an expert of the mechanical and thermal analysis. By their tremendous cooperation, GLIMS mission could pass the numerous reviews. Though many science mission using very small satellite will be planned in near future, strong mutual cooperation between science group and engineering group is important.
  • YAEGASHI Ayumi, SAKANOI Takeshi, KATAOKA Ryuho, ASAMURA Kazushi, KOIWA Aya, SATO Mitsuteru, MIYOSHI Yoshizumi, OKANO Shoichi  極域科学・宙空圏・気水圏・生物・地学シンポジウム講演予稿集(CD−ROM)  2010-  ROMBUNNO.PU01  2010  [Not refereed][Not invited]
  • 八重樫あゆみ, 坂野井健, 片岡龍峰, 浅村和史, 佐藤光輝, 岡野章一  地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD−ROM)  128th-  ROMBUNNO.B006-51  2010  [Not refereed][Not invited]
  • 佐藤 光輝, 牛尾 知雄, 森本 健志, 高橋 幸弘, INAN Umran, 芳原 容英, 菊池 雅行, 鈴木 睦, 山崎 敦, 阿部 琢美, 吉田 和哉, 坂本 祐二, 奥山 圭一, 石田 良平, 河崎 善一郎  大気電気学会誌 = / Society of Atmospheric Electricity of Japan  3-  (2)  60  -61  2009/10/30  [Not refereed][Not invited]
  • 福原 哲哉, 高橋 幸弘, 佐藤 光輝, 渡部 重十, 佐藤 創我, 渡邉 誠  日本惑星科学会秋期講演会予稿集  2009-  2009/09/28  [Not refereed][Not invited]
  • Yoshiya Kawasaki, Mario E. Bertaina, Fumiyoshi Kajino, Mitsuteru Sato, Philippe Gorodetzky  31st International Cosmic Ray Conference, ICRC 2009  2009/01/01  [Not refereed][Not invited]
     
    The Extreme Universe Space Observatory on JEM/EF (JEM-EUSO) is a space mission to study extremely high-energy cosmic rays. The JEM-EUSO instrument is a wide-angle refractive telescope in near-ultraviolet wavelength region to observe timeresolved atmospheric fluorescence images of the extensive air showers from the International Space Station. The focal surface is a spherical curved surface, and its area amounts to about 4.5m2. The focal surface detector is covered with over 5,000 multi-anode photomultipliers (MAPMTs). The focal surface detector consists of Photo-Detector-Modules, each of which consists of 9 Elementary Cells (ECs). The EC contains 4 units of MAPMTs. Therefore, about 1,300 ECs or about 150 PDMs are arranged on the whole of the focal surface of JEM-EUSO. The EC is a basic unit of the MAPMT support structure and the front-end electronics. The PDM is a basic unit of the focal surface structure and the data acquisition system.
  • 牛尾 知雄, 森本 健志, 鈴木 睦, 佐藤 光輝  大気電気学会誌 = / Society of Atmospheric Electricity of Japan  2-  (2)  61  -62  2008/11/05  [Not refereed][Not invited]
  • M. Ohishi, M. Mori, Y. Adachi, A. Asahara, G. V. Bicknell, R. W. Clay, Y. Doi, P. G. Edwards, R. Enomoto, S. Gunji, S. Hara, T. Hara, T. Hattori, Sei Hayashi, Y. Higashi, Y. Hirai, K. Inoue, C. Itoh, S. Kabuki, F. Kaiino, H. Katagiri, A. Kawachi, T. Kifune, R. Kiuchi, H. Kubo, T. Kurihara, R. Kurosaka, J. Kushida, Y. Matsubara, Y. Miyashita, T. Mizukami, R. Mizuniwa, H. Muraishi, Y. Muraki, T. Naito, T. Nakamori, S. Nakano, T. Nakase, D. Nishida, K. Nishijima, N. Sakamoto, Y. Sakamoto, M. Sato, A. Seki, V. Stamatescu, T. Suzuki, D. L. Swaby, T. Tanimori, H. Tanimura, G. J. Thornton, F. Tokanai, K. Tsuchiya, S. Watanabe, Y. Yamada, T. Yamaoka, E. Yamazaki, S. Yanagita, T. Yoshida, T. Yoshikoshi, Y. Yukawa  ASTROPARTICLE PHYSICS  30-  (2)  47  -53  2008/09  [Not refereed][Not invited]
     
    In 2004, we searched for very high energy (VHE) gamma-ray emission from the Galactic Plane using the CANGAROO-III stereoscopic observation system. Two different longitude regions (e = -19 degrees.5 and e = +13 degrees.0) on the Galactic Plane were observed during July and August 2004. We analyzed events that triggered three telescopes aiming to measure the diffuse emission component. No significant signal associated with the Galactic Plane was found from either of the regions. Assuming that the gamma-ray spectrum is described by a single power-law for energies ranging between a few GeV and TeV, lower limits of the power-law spectral indices were found to be 2.2 for both of the regions with a 99.9% confidence level. This result is consistent with the other VHE measurements and constrains a hypothesis in which a very hard (similar to 2.0) cosmic ray electron spectrum was introduced to explain the EGRET GeV anomaly. (C) 2008 Elsevier B.V. All rights reserved.
  • 地上光学・電磁波観測器とMUレーダーを用いた雷活動と電離圏擾乱現象の同時観測
    足立透, 山本衛, 大塚雄一, 高橋幸弘, 佐藤光輝  京都大学生存圏研究所MU共同利用成果報告書  2008  [Not refereed][Not invited]
  • Toshikazu Ebisuzaki, Fumiyoshi Kajino, Motohiko Nagano, Yoshiyuki Takizawa, Yoshiya Kawasaki, Mitsuteru Sato, M. E. Bertaina, Toshiyukj Sawabe, Toru Shibata, Naoto Sakaki, Naoya Inoue, Yukio Uchibori  Energy Budget in the High Energy Universe - Proceedings of the International Workshop  303  -306  2007/12/01  [Not refereed][Not invited]
     
    JEM-EUSO mission is the science mission to detect extreme energy particles with the energy above lom eV from the orbit. It is attached to Japanese experiment module of International Space Station. The outline of the mission is presented in the present paper. Copyright © 2007 by World Scientific Publishing Co. Pvt. Ltd.
  • Y. Takizawa, T. Ebisuzaki, Y. Kawasaki, M. Sato, M. E. Bertaina, H. Ohmori, Y. Takahashi, F. Kajino, M. Nagano, N. Sakaki, N. Inoue, H. Ikeda, Y. Arai, Y. Takahashi, T. Murakami, James H. Adams  NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS  166-  72  -76  2007/04  [Not refereed][Not invited]
     
    EUSO is a super-wide field UV telescope to detect Ultra-High Energy Cosmic-Rays (UHECRs) with energy above 10(20) eV. It is attached to the International Space Station (ISS) and observes fluorescence photons emitted by giant air showers produced by UHECR. The three dimensional development of the shower is reconstructed from a series of images of the shower. Phase-A study of EUSO under the European Space Agency (ESA) has successfully finished in July 2004. The phase-B study, however, has been postponed for a long time because of financial problems in ESA and Italy. Then, Japanese and U.S. teams re-defined EUSO as a mission attached to the Japanese Experiment Module/Exposure Facility of ISS. They renamed it as JEM-EUSO and started the preparation targeting the launch in 2012 in the framework of second phase of JEM/EF utilization. The outline of the mission is presented.
  • Sawabe T, Sasaki A, Kajino F, Ikeda H, Kawasaki Y, Takizawa Y, Sato M, Ebisuzaki T, JEM-EUSO Collaboration  Meeting abstracts of the Physical Society of Japan  62-  (1)  2007/02/28  [Not refereed][Not invited]
  • N. Sakaki, Y. Takizawa, Y. Kawasaki, M. Sato, T. Sawabe, M. Nagano, T. Tsunoda, T. Kamioka, K. Hayasaka, M. Kamimura, A. K. Yoshida, T. Shibata, T. Ebisuzaki, K. Inoue, F. Kajino, Y. Takahashi, Y. Saito, K. Yamada, T. Kawasaki  Proceedings of the 30th International Cosmic Ray Conference, ICRC 2007  5-  (HE PART 2)  965  -968  2007  [Not refereed][Not invited]
     
    Ultra-high energy cosmic rays (UHECRs) above 100 EeV have been observed with several experiments. Their origin and propagation mechanism are still in mystery mainly due to the low statistics. In order to observe UHECRs with sufficient statistics, the JEM-EUSO mission is going on. In the JEMEUSO mission, fluorescence and ̌Cerenkov light from the extensive air showers induced by UHECRs are observed with a telescope attached to the International Space Station. It is important to study the background (BG) intensity in near UV region (300-400nm) seen from the JEM-EUSO telescope. We launched a balloon at Sanriku Balloon Center of JAXA to investigate the nightglow and the clouds on August 29, 2005. The upward and downward nightglow were measured in the eight near UV bands and the cloud images were recorded with an infrared thermography. In this paper, the detail of the experiment and the results will be reported.
  • 内堀幸夫, 北村尚, 大竹奈緒美, 高島健, 梶野文義, 沢辺俊之, 椿智子, 滝澤慶之, 川崎賀也, 佐藤光輝  NIRS-M (National Inst. of Radiological Sciences)  (193)  27  -33  2006/06  [Not refereed][Not invited]
  • 戎崎俊一, 上原嘉宏, 大森整, 川崎賀也, 佐藤光輝, 滝澤慶之, BERTAINA Mario E, 高橋義幸, 梶野文義, 沢辺俊之, 井上覚太, 坂田通徳, 永野元彦, 柴田徹, 榊直人, 井上直也, 内堀幸夫, 高橋幸弘, 新井康夫, 吉田滋, 水本好彦, 井上進, 浅野勝晃, 池田博一, 村上敏夫, 米徳大輔, 伊藤好孝, 長滝重博, 永田真, ADAMS James H  ICRRニュース  (60)  9  -11  2006/05/31  [Not refereed][Not invited]
  • 梶野文義, 沢辺俊之, 椿智子, 滝澤慶之, 川崎賀也, 佐藤光輝, 内堀幸夫, 北村尚  NIRS-M (National Inst. of Radiological Sciences)  (192)  276  -277  2006/05  [Not refereed][Not invited]
  • 沢辺俊之, 椿智子, 梶野文義, 内堀幸夫, 北村尚, 滝澤慶之, 川崎賀也, 佐藤光輝, 戎崎俊一, 佐藤家郷, 礒野成実, JEMEUSO Collaboration  日本物理学会講演概要集  61-  (1)  2006/03/04  [Not refereed][Not invited]
  • R Enomoto, K Tsuchiya, Y Adachi, S Kabuki, PG Edwards, A Asahara, GV Bicknell, RW Clay, Y Doi, S Gunji, S Hara, T Hara, T Hattori, S Hayashi, Y Higashi, R Inoue, C Itoh, F Kajino, H Katagiri, A Kawachi, S Kawasaki, T Kifune, R Kiuchi, K Konno, LT Ksenofontov, H Kubo, J Kushida, Y Matsubara, Y Mizumoto, M Mori, H Muraishi, Y Muraki, T Naito, T Nakamori, D Nishida, K Nishijima, M Ohishi, Patterson, JR, RJ Protheroe, Y Sakamoto, M Sato, S Suzuki, T Suzuki, DL Swaby, T Tanimori, H Tanimura, GJ Thornton, S Watanabe, T Yamaoka, M Yamazaki, S Yanagita, T Yoshida, T Yoshikoshi, M Yuasa, Y Yukawa  ASTROPHYSICAL JOURNAL  638-  (1)  397  -408  2006/02  [Not refereed][Not invited]
     
    We made stereoscopic observations of the Vela pulsar region with two of the 10 m diameter CANGAROO-III imaging atmospheric Cerenkov telescopes in 2004 January and February in a search for sub-TeV gamma rays from the pulsar and surrounding regions. We describe the observations, provide a detailed account of the calibration methods, and introduce the improved and bias-free analysis techniques employed for CANGAROO-III data. No evidence of gamma-ray emission is found from either the pulsar position or the previously reported position offset by 0.degrees 13, and the resulting upper limits are a factor of 5 less than the previously reported flux from observations with the CANGAROO-I 3.8 m telescope. Following the recent report by the H. E. S. S. group of TeV gamma-ray emission from the pulsar wind nebula, which is similar to 0.degrees 5 south of the pulsar position, we examined this region and found supporting evidence for emission extended over similar to 0.degrees 6.
  • 沢辺俊之, 椿智子, 山崎明子, 梶野文義, 内堀幸夫, 北村尚, 滝澤慶之, 川崎賢也, 佐藤光輝, 戎崎俊一, 佐藤家郷, 礒野成実, 他EUSO-JapanCollaboration  日本物理学会講演概要集  60-  (2)  2005/08/19  [Not refereed][Not invited]
  • F. Kajino, T. Sawabe, K. Inoue, Y. Kawasaki, Y. Takizawa, M. Sato, T. Ebisuzaki, Y. Uchihori, I. Sato, N. Isono  Proceedings of the 29th International Cosmic Ray Conference Vol 8: HE 1.5  8-  153  -156  2005  [Not refereed][Not invited]
     
    The focal surface detector of the EUSO telescope consists of a few hundred thousand pixels of photodetectors which are assembled to about 150 photodetector modules (PDM). Multi-channel high voltage power supply (HV PS) system for the MAPMTs used for the detector has been developed. Individual HV PS is installed in each PDM. This system will be used in outer space for 3 years at high altitude of about 420 km. Therefore, various crucial conditions are imposed. Design concept of the HV PS system and some test results are described.
  • Y. Takizawa, Y. Kawasaki, M. Sato, M. E. Bertaina, T. Ebisuzaki, H. A. Shimizu, T. Sawabe, F. Kajino, I. Sato, H. Takara, N. Isono, M. Ameri, S. Cuneo, F. Fontanelli, V. Gracco, P. Musico, M. Pallavicini, A. Petrolini, M. Sannino, F. Siccardi, A. Thea  Proceedings of the 29th International Cosmic Ray Conference Vol 8: HE 1.5  8-  213  -216  2005  [Not refereed][Not invited]
     
    The Focal Surface detector of EUSO (Extreme Universe Space Observatory) consists of small autonomous functional units (elementary cell, EC) assembled in larger modules (Photo Detector Modules, PDM). Each EC is conceived as an array of 4 multianode photomultipliers (MAPMTs). We have developed EC structure for the current baseline of the multianode photomultiplier (MAPMT, R8900-M36). As the mechanical characteristics of the PDM structure (e.g. robustness to thermal and launch shocks, vibrations at launch) will affect the EC structure, we have also built a trial PDM, consisting of 36 MAPMTs (9 ECs) arranged in a cartesian layout. The purpose of such trial PDM is to develop and optimize the EC structure.
  • Y. Uchihori, F. Kajino, T. Sawabe, Y. Kawasaki, Y. Takizawa, M. Sato, T. Ebisuzaki  Proceedings of the 29th International Cosmic Ray Conference Vol 8: HE 1.5  8-  237  -240  2005  [Not refereed][Not invited]
     
    The EUSO telescope will be irradiated with space radiation for 5 years while on a low earth orbit. Many parts of the telescope are of a new design and have no data regarding radiation damage. In order to investigate the effects of radiation damage to the electric parts while in a low earth orbit, photodetector modules (PDM) [1] and glass windows for the Multi-Anode Photo-Multiplier Tubes (MAPMT) in the telescope [2] were irradiated with medium energy (70 MeV) proton beams from an accelerator at the National Institute of Radiological Sciences (NIRS) in Japan. Based on these results, the capability of these parts when exposed to an actual space radiation environment after 5 years can be estimated.
  • Y. Kawasaki, M. E. Bertaina, N. Sakaki, M. Sato, H. M. Shimizu, Y. Takizawa, Y. Uchihori, N. Inoue, I. Ohtsu, K. Inoue, T. Sawabe, F. Kajino  Proceedings of the 29th International Cosmic Ray Conference Vol 8: HE 1.5  8-  165  -168  2005  [Not refereed][Not invited]
     
    The focal surface of the EUSO telescope consists of a few hundred thousand of pixels of photo-detectors and detects air showers as mosaic images. The strongest requirement for the focal surface detector is the maximization of the photon detection efficiency together with the uniformity over the focal surface. We have developed a new type of multi-anode photomultiplier tube (MAPMT). The tatal photon detection efficiency has improved than before by about 2.1 times.
  • 日本に発生する冬季スプライトと雷雲に関する研究
    足立透, 福西浩, 高橋幸弘, 佐藤光輝  第18回大気圏シンポジウム原稿集  2004  [Not refereed][Not invited]

Industrial Property Rights

  • 2921887:Lightning-strike Electric Charge Estimation System and Method    2018/07/04
    Honma N, Y. Hongo, Y. Takahashi, M. Sato, F. Tsuchiya, D. Tsurushima
  • 特許第6067741号:落雷の電荷量推定システム、落雷の電荷量推定方法、及び、プログラム    2017/01/06
    本間規泰, 本郷保二, 高橋幸弘, 佐藤光輝, 土屋史紀, 鶴島大樹

Awards & Honors

  • 2016/04 The Institute of Electrical Engineers of Japan 72nd Technical Development Award
     JEM-GLIMS Observations of Lightning and TLEs from the ISS 
    受賞者: Mitsuteru SATO;Tomoo USHIO;Takeshi MORIMOTO;Makoto SUZUKI;Masayuki KIKUCHI
  • 2014/06 アメリカ宇宙航行学会 Top Discoveries in Microgravity
     JEM-GLIMS: First Qualitative Nadir Observations of Lightning and TLEs from ISS/JEM 
    受賞者: Mitsuteru SATO
  • 2013/06 WNI WxBunka Foundaton 3rd Weather Culture Award
     雷放電・大気電場観測による極端突発気象現象の予測 
    受賞者: Mitsuteru SATO
  • 2012/05 WNI WxBunka Foundaton 2nd Weather Culture Award
     「雷放電及び大気電場観測によるゲリラ雷雨・落雷の予測 
    受賞者: Mitsuteru SATO

Research Grants & Projects

  • Development of Extreme Weather Monitoring and Information Sharing System in the Philippines
    JICA, JST:SATREPS
    Date (from‐to) : 2016/06 -2022/03 
    Author : TAKAHASHI Yukihiro
  • Let's monitor thunderstorm activity in Southeast Asia using hand-made radio receiver
    JSPS:hirameki☆tokimeki science
    Date (from‐to) : 2019/04 -2020/10 
    Author : TAKAHASHI Yukihiro
  • Identification of Generation/Driving Mechanisms of Upper-Atmospheric Discharges and Global Electric Circuit Using Satellite Data and Numerical Simulation
    JSPS:科学研究費補助金・基盤研究(B)(一般)
    Date (from‐to) : 2016/04 -2019/03 
    Author : SATO Mitsuteru
  • Monitoring and Prediction of Extreme Weather Using Lightning Detection Network and Micro-Satellites
    JSPS:e-ASIA Program
    Date (from‐to) : 2015 -2018 
    Author : TAKAHASHI Yukihiro
  • Identification of the Occurrence Conditions and Mechanisms of Transient Luminous Events from Space- and Ground-Based Observations
    JSPS:Grant-in-Aid for Scientific Research (B)
    Date (from‐to) : 2012/04 -2016/03 
    Author : SATO Mitsuteru
  • Observation of Thunderstorm Electrical Structure and Modeling
    JSPS:Grant-in-Aid for Scientific Research (B)
    Date (from‐to) : 2010/04 -2013/03 
    Author : USHIO Tomoo
  • Detailed Design of Electronics Circuit of Photometer Flight Model onboard TARANIS satellite
    ISAS, JAXA:国際共同ミッション推進研究
    Date (from‐to) : 2012/01 -2012/03 
    Author : SATO Mitsuteru
  • 小型衛星による宇宙空間からのスプライト・地球ガンマ線観測と発生機構の解明
    北海道大学:総長室重点配分経費
    Date (from‐to) : 2008/04 -2009/03 
    Author : 佐藤光輝
  • マイクロサテライトが拓くスプライト及び雷放電逃走電子の科学
    JSPS:Grant-in-Aid for Scientific Research (A)
    Date (from‐to) : 2005/04 -2009/03 
    Author : TAKAHASHI Yukihiro
  • Development of Photometers onboard TARANIS Satellite
    ISAS, JAXA:国際共同ミッション推進研究
    Date (from‐to) : 2007/04 -2008/03 
    Author : SATO Mitsuteru
  • 高高度雷放電および地球ガンマ線観測用小型フィルタフォトメータの開発
    ISAS, JAXA:国際共同ミッション推進研究
    Date (from‐to) : 2006/04 -2007/03 
    Author : 佐藤光輝
  • 宇宙空間からの超高層雷放電観測にむけた広視野望遠鏡検出器制御システムの開発
    JSPS:Grant-in-Aid for Young Scientists (B)
    Date (from‐to) : 2005/04 -2007/03 
    Author : SATO Mitsuteru

Educational Activities

Teaching Experience

  • Planetary Atmospheric Sciences 2
    開講年度 : 2018
    課程区分 : 修士課程
    開講学部 : 理学院
    キーワード : プラズマ,電離圏・磁気圏,ドリフト運動,断熱不変量,放射線帯,電磁流体方程式(MHD),電磁圏電流系,ストーム,サブストーム
  • Electromagnetism for Earth and Planetary Sciences
    開講年度 : 2018
    課程区分 : 学士課程
    開講学部 : 理学部
    キーワード : 電磁気学,地球惑星科学,地磁気,電磁波,放電,プラズマ,電磁場計測方法


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